1
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Wilkins OH, Blake GA. New interstellar laboratories in the molecular ring. Faraday Discuss 2023; 245:138-163. [PMID: 37394909 DOI: 10.1039/d3fd00003f] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 09/21/2023]
Abstract
Much of what is known about chemistry in star-forming regions comes from observations of nearby (d < 500 pc) low-mass protostars. For chemistry in high-mass star-forming regions, several more distant (d ∼ 2-8 kpc), exceptionally bright molecular sources have also been the subjects of repeated observations but with concomitantly poorer linear spatial resolution. Facilities such as ALMA and JWST, however, now provide the means for observing distant sources at dramatically higher spatial resolution and sensitivity. We used the modest resolving power of the Atacama Compact Array, a dedicated subset of ALMA antennas, to carry out a pilot survey of 11 giant molecular clouds selected from the Bolocam Galactic Plane Survey [Battisti & Heyer, Astrophys. J., 2014, 780, 173] within the so-called molecular ring between about 4 and 8 kpc from the galactic center. Within our observed sample, molecular emission regions-most of which correspond to at least one (candidate) young stellar object-exhibit a range of chemical complexity and diversity. Furthermore, nine target giant molecular clouds contain well-fit methanol emission, giving us a first look at the spatial chemical variability within the objects at relatively high (compared to past observations) resolutions of ∼5''. This work lays the foundation for future high angular resolution studies of gas-phase chemistry with the full ALMA.
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Affiliation(s)
- Olivia H Wilkins
- California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
| | - Geoffrey A Blake
- California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
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2
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Mahjoub A, Altwegg K, Poston MJ, Rubin M, Hodyss R, Choukroun M, Ehlmann BL, Hänni N, Brown ME, Blacksberg J, Eiler JM, Hand KP. Complex organosulfur molecules on comet 67P: Evidence from the ROSINA measurements and insights from laboratory simulations. Sci Adv 2023; 9:eadh0394. [PMID: 37285429 DOI: 10.1126/sciadv.adh0394] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/07/2023] [Accepted: 05/01/2023] [Indexed: 06/09/2023]
Abstract
The ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) instrument aboard the Rosetta mission revolutionized our understanding of cometary material composition. One of Rosetta's key findings is the complexity of the composition of comet 67P/Churyumov-Gerasimenko. Here, we used ROSINA data to analyze dust particles that were volatilized during a dust event in September 2016 and report the detection of large organosulfur species and an increase in the abundances of sulfurous species previously detected in the coma. Our data support the presence of complex sulfur-bearing organics on the surface of the comet. In addition, we conducted laboratory simulations that show that this material may have formed from chemical reactions that were initiated by the irradiation of mixed ices containing H2S. Our findings highlight the importance of sulfur chemistry in cometary and precometary materials and the possibility of characterizing organosulfur materials in other comets and small icy bodies using the James Webb Space Telescope.
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Affiliation(s)
- Ahmed Mahjoub
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
- Space Science Institute, 4765 Walnut St, Suite B, Boulder, CO 80301, USA
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Bern, Switzerland
| | | | - Martin Rubin
- Physikalisches Institut, University of Bern, Bern, Switzerland
| | - Robert Hodyss
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Mathieu Choukroun
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Bethany L Ehlmann
- Division of Planetary and Space Sciences, Caltech, Pasadena, CA 91125, USA
| | - Nora Hänni
- Physikalisches Institut, University of Bern, Bern, Switzerland
| | - Michael E Brown
- Division of Planetary and Space Sciences, Caltech, Pasadena, CA 91125, USA
| | - Jordana Blacksberg
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - John M Eiler
- Division of Planetary and Space Sciences, Caltech, Pasadena, CA 91125, USA
| | - Kevin P Hand
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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3
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Yang D, Lian J, Zhao X, Hou Q, Chen Y, Zhang Y. A mathematical model for supercooling process and its application to frazil ice evolution. Sci Rep 2023; 13:5801. [PMID: 37037896 PMCID: PMC10086004 DOI: 10.1038/s41598-023-33097-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/14/2022] [Accepted: 04/07/2023] [Indexed: 04/12/2023] Open
Abstract
The calculation of the number of ice crystals for the model of frazil ice evolution is very important and affects the whole frazil events. In this paper, the general formula for the number of frazil ice crystals was established considering secondary nucleation, flocculation, gravity and turbulent entrainment, and ice crystals by melting. Meanwhile, two physical processes of secondary nucleation and flocculation were expressed by introducing critical impact velocity and the probability of flocculation from previous models. It has been found that the simulation results of frazil ice evolution are in good agreement with the experimental data and actual project. Then, Sobol method is carried out to judge parameters' influence degree, which found the number of nuclei produced [Formula: see text] is the most sensitive and has the greatest influence on the model results. In addition, sensitivity analysis of these parameters shows that they can affect the maximum supercooling and the period of supercooling. Therefore, the calculation method of the number of ice crystals is applied, which provides technical support for exploring the water temperature and internal relationship of frazil ice evolution.
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Affiliation(s)
- Deming Yang
- State Key Laboratory of Hydraulic Engineering Simulation and Safety, Tianjin University, Tianjin, China
- School of Civil Engineering, Tianjin University, Tianjin, China
| | - Jijian Lian
- State Key Laboratory of Hydraulic Engineering Simulation and Safety, Tianjin University, Tianjin, China
- School of Civil Engineering, Tianjin University, Tianjin, China
| | - Xin Zhao
- State Key Laboratory of Hydraulic Engineering Simulation and Safety, Tianjin University, Tianjin, China.
- School of Civil Engineering, Tianjin University, Tianjin, China.
| | - Qingzhi Hou
- State Key Laboratory of Hydraulic Engineering Simulation and Safety, Tianjin University, Tianjin, China
- School of Civil Engineering, Tianjin University, Tianjin, China
| | - Yunfei Chen
- State Key Laboratory of Hydraulic Engineering Simulation and Safety, Tianjin University, Tianjin, China
- School of Civil Engineering, Tianjin University, Tianjin, China
| | - Yue Zhang
- State Key Laboratory of Hydraulic Engineering Simulation and Safety, Tianjin University, Tianjin, China
- School of Civil Engineering, Tianjin University, Tianjin, China
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4
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Fujishiro K, Morinaka Y, Ono Y, Tanaka T, Scott LT, Ito H, Itami K. Lithium-Mediated Mechanochemical Cyclodehydrogenation. J Am Chem Soc 2023; 145:8163-8175. [PMID: 37011146 DOI: 10.1021/jacs.3c01185] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/05/2023]
Abstract
Cyclodehydrogenation is an essential synthetic method for the preparation of polycyclic aromatic hydrocarbons, polycyclic heteroaromatic compounds, and nanographenes. Among the many examples, anionic cyclodehydrogenation using potassium(0) has attracted synthetic chemists because of its irreplaceable reactivity and utility in obtaining rylene structures from binaphthyl derivatives. However, existing methods are difficult to use in terms of practicality, pyrophoricity, and lack of scalability and applicability. Herein, we report the development of a lithium(0)-mediated mechanochemical anionic cyclodehydrogenation reaction for the first time. This reaction could be easily performed using a conventional and easy-to-handle lithium(0) wire at room temperature, even under air, and the reaction of 1,1'-binaphthyl is complete within 30 min to afford perylene in 94% yield. Using this novel and user-friendly protocol, we investigated substrate scope, reaction mechanism, and gram-scale synthesis. As a result, remarkable applicability and practicality over previous methods, as well as limitations, were comprehensively studied by computational studies and nuclear magnetic resonance analysis. Furthermore, we demonstrated two-, three-, and five-fold cyclodehydrogenations for the synthesis of novel nanographenes. In particular, quinterrylene ([5]rylene or pentarylene), the longest nonsubstituted molecular rylene, was synthesized for the first time.
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Affiliation(s)
- Kanna Fujishiro
- Department of Chemistry, Graduate School of Science, Nagoya University, Nagoya 464-8602, Japan
| | - Yuta Morinaka
- Tokyo Research Center, Organic Materials Research Laboratory, Tosoh Corporation, 2743-1 Hayakawa, Ayase, Kanagawa 252-1123, Japan
| | - Yohei Ono
- Tokyo Research Center, Organic Materials Research Laboratory, Tosoh Corporation, 2743-1 Hayakawa, Ayase, Kanagawa 252-1123, Japan
| | - Tsuyoshi Tanaka
- Tosoh Corporation, 3-8-2 Shiba, Minato-ku, Tokyo 105-8623, Japan
| | - Lawrence T Scott
- Department of Chemistry, University of Nevada, Reno, Nevada 89557-0216, United States
| | - Hideto Ito
- Department of Chemistry, Graduate School of Science, Nagoya University, Nagoya 464-8602, Japan
| | - Kenichiro Itami
- Department of Chemistry, Graduate School of Science, Nagoya University, Nagoya 464-8602, Japan
- Institute of Transformative Bio-Molecules (WPI-ITbM), Nagoya University, Nagoya 464-8602, Japan
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5
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Chen YC, Liu X, Foord A, Shen Y, Oguri M, Chen N, Di Matteo T, Holgado M, Hwang HC, Zakamska N. A close quasar pair in a disk-disk galaxy merger at z = 2.17. Nature 2023; 616:45-49. [PMID: 37020007 DOI: 10.1038/s41586-023-05766-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/13/2022] [Accepted: 01/26/2023] [Indexed: 04/07/2023]
Abstract
Galaxy mergers produce pairs of supermassive black holes (SMBHs), which may be witnessed as dual quasars if both SMBHs are rapidly accreting. The kiloparsec (kpc)-scale separation represents a physical regime sufficiently close for merger-induced effects to be important1 yet wide enough to be directly resolvable with the facilities currently available. Whereas many kpc-scale, dual active galactic nuclei-the low-luminosity counterparts of quasars-have been observed in low-redshift mergers2, no unambiguous dual quasar is known at cosmic noon (z ≈ 2), the peak of global star formation and quasar activity3,4. Here we report multiwavelength observations of Sloan Digital Sky Survey (SDSS) J0749 + 2255 as a kpc-scale, dual-quasar system hosted by a galaxy merger at cosmic noon (z = 2.17). We discover extended host galaxies associated with the much brighter compact quasar nuclei (separated by 0.46″ or 3.8 kpc) and low-surface-brightness tidal features as evidence for galactic interactions. Unlike its low-redshift and low-luminosity counterparts, SDSS J0749 + 2255 is hosted by massive compact disk-dominated galaxies. The apparent lack of stellar bulges and the fact that SDSS J0749 + 2255 already follows the local SMBH mass-host stellar mass relation, suggest that at least some SMBHs may have formed before their host stellar bulges. While still at kpc-scale separations where the host-galaxy gravitational potential dominates, the two SMBHs may evolve into a gravitationally bound binary system in around 0.22 Gyr.
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Affiliation(s)
- Yu-Ching Chen
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
- National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Champaign, IL, USA
| | - Xin Liu
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA.
- National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Champaign, IL, USA.
| | - Adi Foord
- Kavli Institute of Particle Astrophysics and Cosmology, Stanford University, Stanford, CA, USA
| | - Yue Shen
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
- National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Champaign, IL, USA
| | - Masamune Oguri
- Center for Frontier Science, Chiba University, Chiba, Japan
- Department of Physics, Graduate School of Science, Chiba University, Chiba, Japan
| | - Nianyi Chen
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
| | - Tiziana Di Matteo
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
- NSF AI Planning Institute for Physics of the Future, Carnegie Mellon University, Pittsburgh, PA, USA
- OzGrav-Melbourne, Australian Research Council Centre of Excellence for Gravitational Wave Discovery, Melbourne, Victoria, Australia
| | - Miguel Holgado
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
| | - Hsiang-Chih Hwang
- School of Natural Sciences, Institute for Advanced Study, Princeton, NJ, USA
| | - Nadia Zakamska
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
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6
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Raymond SN. Earth's molten youth had long-lasting consequences. Nature 2023; 616:251-252. [PMID: 37045915 DOI: 10.1038/d41586-023-00979-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/14/2023]
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7
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Beom Jo Y, Park SH, Soo Kim E. Lagrangian computational fluid dynamics for nuclear Thermal-Hydraulics & safety. Nuclear Engineering and Design 2023. [DOI: 10.1016/j.nucengdes.2023.112228] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/27/2023]
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8
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Jani pour H, Noorbala MR, Namazian M. Intermolecular potential energy surfaces of NeH3+ and ArH3+ systems using ab initio methods. COMPUT THEOR CHEM 2023. [DOI: 10.1016/j.comptc.2023.114050] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
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9
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Di Mascolo L, Saro A, Mroczkowski T, Borgani S, Churazov E, Rasia E, Tozzi P, Dannerbauer H, Basu K, Carilli CL, Ginolfi M, Miley G, Nonino M, Pannella M, Pentericci L, Rizzo F. Forming intracluster gas in a galaxy protocluster at a redshift of 2.16. Nature 2023; 615:809-812. [PMID: 36991192 DOI: 10.1038/s41586-023-05761-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/28/2022] [Accepted: 01/25/2023] [Indexed: 03/30/2023]
Abstract
AbstractGalaxy clusters are the most massive gravitationally bound structures in the Universe, comprising thousands of galaxies and pervaded by a diffuse, hot intracluster medium (ICM) that dominates the baryonic content of these systems. The formation and evolution of the ICM across cosmic time1 is thought to be driven by the continuous accretion of matter from the large-scale filamentary surroundings and energetic merger events with other clusters or groups. Until now, however, direct observations of the intracluster gas have been limited only to mature clusters in the later three-quarters of the history of the Universe, and we have been lacking a direct view of the hot, thermalized cluster atmosphere at the epoch when the first massive clusters formed. Here we report the detection (about 6σ) of the thermal Sunyaev–Zeldovich (SZ) effect2 in the direction of a protocluster. In fact, the SZ signal reveals the ICM thermal energy in a way that is insensitive to cosmological dimming, making it ideal for tracing the thermal history of cosmic structures3. This result indicates the presence of a nascent ICM within the Spiderweb protocluster at redshift z = 2.156, around 10 billion years ago. The amplitude and morphology of the detected signal show that the SZ effect from the protocluster is lower than expected from dynamical considerations and comparable with that of lower-redshift group-scale systems, consistent with expectations for a dynamically active progenitor of a local galaxy cluster.
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10
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Clues to the assembly of an infant galaxy cluster. Nature 2023. [PMID: 36991047 DOI: 10.1038/d41586-023-00875-8] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/31/2023]
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11
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Lykawka PS, Ito T. Terrestrial planet and asteroid belt formation by Jupiter-Saturn chaotic excitation. Sci Rep 2023; 13:4708. [PMID: 36973305 PMCID: PMC10042868 DOI: 10.1038/s41598-023-30382-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/21/2022] [Accepted: 02/21/2023] [Indexed: 03/29/2023] Open
Abstract
The terrestrial planets formed by accretion of asteroid-like objects within the inner solar system's protoplanetary disk. Previous works have found that forming a small-mass Mars requires the disk to contain little mass beyond ~ 1.5 au (i.e., the disk mass was concentrated within this boundary). The asteroid belt also holds crucial information about the origin of such a narrow disk. Several scenarios may produce a narrow disk. However, simultaneously replicating the four terrestrial planets and the inner solar system properties remains elusive. Here, we found that chaotic excitation of disk objects generated by a near-resonant configuration of Jupiter-Saturn can create a narrow disk, allowing the formation of the terrestrial planets and the asteroid belt. Our simulations showed that this mechanism could typically deplete a massive disk beyond ~ 1.5 au on a 5-10 Myr timescale. The resulting terrestrial systems reproduced the current orbits and masses of Venus, Earth and Mars. Adding an inner region disk component within ~ 0.8-0.9 au allowed several terrestrial systems to simultaneously form analogues of the four terrestrial planets. Our terrestrial systems also frequently satisfied additional constraints: Moon-forming giant impacts occurring after a median ~ 30-55 Myr, late impactors represented by disk objects formed within 2 au, and effective water delivery during the first 10-20 Myr of Earth's formation. Finally, our model asteroid belt explained the asteroid belt's orbital structure, small mass and taxonomy (S-, C- and D/P-types).
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Affiliation(s)
| | - Takashi Ito
- Center for Computational Astrophysics, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo, 181-8588, Japan
- Planetary Exploration Research Center, Chiba Institute of Technology, 2-17-1 Tsudanuma, Narashino, Chiba, 275-0016, Japan
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12
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Capolupo A, Quaranta A, Serao R. Field Mixing in Curved Spacetime and Dark Matter. Symmetry (Basel) 2023. [DOI: 10.3390/sym15040807] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/29/2023] Open
Abstract
An extensive review of recent results concerning the quantum field theory of particle mixing in curved spacetime is presented. The rich mathematical structure of the theory for both fermions and bosons, stemming from the interplay of curved space quantization and field mixing, is discussed, and its phenomenological implications are shown. Fermionic and bosonic oscillation formulae for arbitrary globally hyperbolic spacetimes are derived and the transition probabilities are explicitly computed on some metrics of cosmological and astrophysical interest. The formulae thus obtained are characterized by a pure QFT correction to the amplitudes, which is absent in quantum mechanics, where only the phase of the oscillations is affected by the gravitational background. Their deviation from the flat space probabilities is demonstrated, with the aid of numerical analyses. The condensate structure of the flavor vacuum of mixed fermions is studied, assessing its role as a possible dark matter component in a cosmological context. It is shown that the flavor vacuum behaves as a barotropic fluid, satisfying the equation of the state of cold dark matter. New experiments on the cosmic neutrino background, as PTOLEMY, may validate these theoretical results.
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13
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Hansen K, Licht O, Kurbanov A, Toker Y. Cascade Infrared Thermal Photon Emission. J Phys Chem A 2023; 127:2889-2894. [PMID: 36966418 DOI: 10.1021/acs.jpca.2c09024] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/27/2023]
Abstract
The later stages of cooling of molecules and clusters in the interstellar medium are dominated by emission of vibrational infrared radiation. With the development of cryogenic storage it has become possible to experimentally study these processes. Recent storage ring results demonstrate that intramolecular vibrational redistribution takes place within the cooling process, and an harmonic cascade model has been used to interpret the data. Here we analyze this model and show that the energy distributions and the photon emission rates develop into near-universal functions that can be characterized with only a few parameters, irrespective of the precise vibrational spectra and oscillator strengths of the systems. We show that the photon emission rate and emitted power vary linearly with total excitation energy with a small offset. The time developments of ensemble internal energy distributions are calculated with respect to their first two moments. The excitation energy decreases exponentially with a rate constant which is the average of all k1→0 Einstein coefficients, and the time development of the variance is also calculated.
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Affiliation(s)
- Klavs Hansen
- Lanzhou Center for Theoretical Physics, Key Laboratory of Theoretical Physics of Gansu Province, Lanzhou University, Lanzhou, Gansu 730000, China
- Center for Joint Quantum Studies and Department of Physics, School of Science, Tianjin University, 92 Weijin Road, Tianjin 300072, China
| | - Ori Licht
- Department of Physics and Institute for Nanotechnology and Advanced Materials, Bar Ilan University, Ramat-Gan 5290002, Israel
| | - Adeliya Kurbanov
- Department of Physics and Institute for Nanotechnology and Advanced Materials, Bar Ilan University, Ramat-Gan 5290002, Israel
| | - Yoni Toker
- Department of Physics and Institute for Nanotechnology and Advanced Materials, Bar Ilan University, Ramat-Gan 5290002, Israel
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14
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Bueno de Mesquita CP, Wu D, Tringe SG. Methyl-Based Methanogenesis: an Ecological and Genomic Review. Microbiol Mol Biol Rev 2023; 87:e0002422. [PMID: 36692297 PMCID: PMC10029344 DOI: 10.1128/mmbr.00024-22] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/25/2023] Open
Abstract
Methyl-based methanogenesis is one of three broad categories of archaeal anaerobic methanogenesis, including both the methyl dismutation (methylotrophic) pathway and the methyl-reducing (also known as hydrogen-dependent methylotrophic) pathway. Methyl-based methanogenesis is increasingly recognized as an important source of methane in a variety of environments. Here, we provide an overview of methyl-based methanogenesis research, including the conditions under which methyl-based methanogenesis can be a dominant source of methane emissions, experimental methods for distinguishing different pathways of methane production, molecular details of the biochemical pathways involved, and the genes and organisms involved in these processes. We also identify the current gaps in knowledge and present a genomic and metagenomic survey of methyl-based methanogenesis genes, highlighting the diversity of methyl-based methanogens at multiple taxonomic levels and the widespread distribution of known methyl-based methanogenesis genes and families across different environments.
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Affiliation(s)
- Clifton P Bueno de Mesquita
- Department of Energy Joint Genome Institute, Lawrence Berkeley National Laboratory, Berkeley, California, USA
| | - Dongying Wu
- Department of Energy Joint Genome Institute, Lawrence Berkeley National Laboratory, Berkeley, California, USA
| | - Susannah G Tringe
- Department of Energy Joint Genome Institute, Lawrence Berkeley National Laboratory, Berkeley, California, USA
- Environmental Genomics and Systems Biology Division, Lawrence Berkeley National Laboratory, Berkeley, California, USA
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15
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Leboucher H, Simon A, Rapacioli M. Structures and stabilities of PAH clusters solvated by water aggregates: The case of the pyrene dimer. J Chem Phys 2023; 158:114308. [PMID: 36948831 DOI: 10.1063/5.0139482] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/02/2023] Open
Abstract
Although clusters made of polycyclic aromatic hydrocarbon and water monomers are relevant objects in both atmospheric and astrophysical science, little is known about their energetic and structural properties. In this work, we perform global explorations of the potential energy landscapes of neutral clusters made of two pyrene units and one to ten water molecules using a density-functional-based tight-binding (DFTB) potential followed by local optimizations at the density-functional theory level. We discuss the binding energies with respect to various dissociation channels. It shows that cohesion energies of the water clusters interacting with a pyrene dimer are larger than those of the pure water clusters, reaching for the largest clusters an asymptotic limit similar to that of pure water clusters and that, although the hexamer and octamer can be considered magic numbers for isolated water clusters, it is not the case anymore when they are interacting with a pyrene dimer. Ionization potentials are also computed by making use of the configuration interaction extension of DFTB, and we show that in cations, the charge is mostly carried by the pyrene molecules.
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Affiliation(s)
- H Leboucher
- Laboratoire de Chimie et Physique Quantiques LCPQ/FERMI, UMR5626, Université de Toulouse (UPS) and CNRS, 118 Route de Narbonne, F-31062 Toulouse, France
| | - A Simon
- Laboratoire de Chimie et Physique Quantiques LCPQ/FERMI, UMR5626, Université de Toulouse (UPS) and CNRS, 118 Route de Narbonne, F-31062 Toulouse, France
| | - M Rapacioli
- Laboratoire de Chimie et Physique Quantiques LCPQ/FERMI, UMR5626, Université de Toulouse (UPS) and CNRS, 118 Route de Narbonne, F-31062 Toulouse, France
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16
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Francis TA, Maynard-Casely HE, Cable ML, Hodyss R, Ennis C. Simulation of Cocrystal Formation in Planetary Atmospheres: The C 6H 6:C 2H 2 Cocrystal Produced by Gas Deposition. J Phys Chem A 2023; 127:2322-2335. [PMID: 36790472 DOI: 10.1021/acs.jpca.2c08791] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/16/2023]
Abstract
The formation of molecular cocrystals in condensed aerosol particles has been recently proposed as an efficient pathway for generation of complex organics in Titan's atmosphere. It follows that cocrystal precipitation may facilitate the transport of biologically important precursors to the surface to be sequestered in an organic karstic and sand environment. Recent laboratory studies on these planetary minerals have predominantly synthesized cocrystals by the controlled freezing of binary mixtures from the liquid phase, allowing for their structural and spectroscopic characterization. However, these techniques are perhaps not best representative of aerosol nucleation and growth microphysics in planetary atmospheres. Herein, we report the first synthesis of the known 1:1 C6H6:C2H2 cocrystal using vapor deposition methods onto a cryogenically cooled substrate. Subsequent transmission FTIR spectroscopy has confirmed the formation of the empirical C6H6:C2H2 cocrystal structure via the observation of diagnostic infrared spectral features. Predicted by periodic-DFT calculations, altered vibrational profiles depict a changing site symmetry of the C6H6 and C2H2 components after transition to the cocrystal unit cell geometry. The 80 K temperature of the cocrystal phase transition overlaps with the condensation curves obtained for both species in Titan's lower stratosphere, revealing that the cocrystal may act as an important environment for photo- and radio-lytic processes leading to the formation of higher order organics in Titan's atmosphere. Such solid-state astrochemistry can now be pursued in oxygen-free laboratory settings under (ultra)high vacuum using standard surface science setups.
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Affiliation(s)
- Tait A Francis
- Department of Chemistry, University of Otago, Dunedin 9054, New Zealand
| | - Helen E Maynard-Casely
- Australian Nuclear Science and Technology Organisation, Kirrawee, New South Wales 2232, Australia
| | - Morgan L Cable
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109, United States
| | - Robert Hodyss
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109, United States
| | - Courtney Ennis
- Department of Chemistry, University of Otago, Dunedin 9054, New Zealand.,MacDiarmid Institute for Advanced Materials and Nanotechnology, Wellington 6140, New Zealand
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17
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Randi PAS, Pastega DF, Bettega MHF, Jones NC, Hoffmann SV, Eden S, Souza Barbosa A, Limão-Vieira P. Electronically excited states of formic acid investigated by theoretical and experimental methods. Spectrochim Acta A Mol Biomol Spectrosc 2023; 289:122237. [PMID: 36535224 DOI: 10.1016/j.saa.2022.122237] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/01/2022] [Revised: 12/07/2022] [Accepted: 12/10/2022] [Indexed: 06/17/2023]
Abstract
Absolute cross-section values are reported from high-resolution vacuum ultraviolet (VUV) photoabsorption measurements of gas-phase formic acid (HCOOH) in the photon energy range 4.7-10.8 eV (265-115 nm), together with quantum chemical calculations to provide vertical energies and oscillator strengths. The combination of experimental and theoretical methods has allowed a comprehensive assignment of the electronic transitions. The VUV spectrum reveals various vibronic features not previously reported in the literature, notably associated with (3pa'←10a'), (3p'a'←10a'), (3sa'←2a″) and (3pa'←2a″) Rydberg transitions. The assignment of vibrational features in the absorption bands reveal that the C=O stretching, v3'a', the H'-O-C' deformation, v5'a', the C-O stretching, v6'a', and the O=C-O' deformation, v7'a' modes are mainly active. The measured absolute photoabsorption cross sections have also been used to estimate the photolysis lifetime of HCOOH in the upper stratosphere (30-50 km), showing that solar photolysis is an important sink at altitudes above 30 km but not in the troposphere. Potential energy curves for the lowest-lying electronic excited states, as a function of the C=O coordinate, are obtained employing time dependent density functional theory (TD-DFT). These calculations have shown the relevance of internal conversion from Rydberg to valence character governing the nuclear dynamics, yielding clear evidence of the rather complex multidimensional nature of the potential energy surfaces involved.
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Affiliation(s)
- P A S Randi
- Departamento de Física, Universidade Federal do Paraná, Caixa Postal 19044, 81531-980 Curitiba, Paraná, Brazil
| | - D F Pastega
- Departamento de Física, Universidade Federal do Paraná, Caixa Postal 19044, 81531-980 Curitiba, Paraná, Brazil
| | - M H F Bettega
- Departamento de Física, Universidade Federal do Paraná, Caixa Postal 19044, 81531-980 Curitiba, Paraná, Brazil
| | - N C Jones
- ISA, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000, Aarhus C, Denmark
| | - S V Hoffmann
- ISA, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000, Aarhus C, Denmark
| | - S Eden
- School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
| | - A Souza Barbosa
- Departamento de Física, Universidade Federal do Paraná, Caixa Postal 19044, 81531-980 Curitiba, Paraná, Brazil.
| | - P Limão-Vieira
- Departamento de Física, Universidade Federal do Paraná, Caixa Postal 19044, 81531-980 Curitiba, Paraná, Brazil; Atomic and Molecular Collisions Laboratory, CEFITEC, Department of Physics, NOVA School of Science and Technology, Universidade NOVA de Lisboa, 2829-516 Caparica, Portugal.
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18
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Joshi PR, Tsuge M, Tseng CY, Lee YP. Infrared spectra of isoquinolinium (iso-C 9H 7NH +) and isoquinolinyl radicals (iso-C 9H 7NH and 1-, 3-, 4-, 5-, 6-, 7- and 8-iso-HC 9H 7N) isolated in solid para-hydrogen. Phys Chem Chem Phys 2023; 25:11934-11950. [PMID: 36916330 DOI: 10.1039/d3cp00246b] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/22/2023]
Abstract
Protonated polycyclic aromatic nitrogen heterocycles (H+PANH) are prospective candidates that may contribute to interstellar unidentified infrared (UIR) emission bands because protonation enhances the relative intensities of the bands near 6.2, 7.7 and 8.6 μm, and the presence of the N atom induces a blue shift of the ring-stretching modes so that the spectra of H+PANH match better with the 6.2 μm feature in class-A UIR spectra. We report the infrared (IR) spectra of protonated isoquinoline (the 2-isoquinolinium cation, iso-C9H7NH+), its neutral counterpart (the 2-isoquinolinyl radical, iso-C9H7NH), and another mono-hydrogenated product (the 6-isoquinolinyl radical, 6-iso-HC9H7N), produced on the electron-bombardment of a mixture of isoquinoline (iso-C9H7N) with excess para-hydrogen (p-H2) during matrix deposition at 3.2 K. To generate additional isomers of hydrogenated isoquinoline, we irradiated iso-C9H7N/Cl2/p-H2 matrices at 365 nm to generate Cl atoms, followed by IR irradiation to generate H atoms via Cl + H2 (v = 1) → HCl + H; the H atoms thus generated reacted with iso-C9H7N. In addition to iso-C9H7NH and 6-iso-HC9H7N observed in the electron-bombardment experiments, we identified six additional hydrogenated isoquinoline species, 1-, 3-, 4-, 5-, 7- and 8-iso-HC9H7N, via their IR spectra; hydrogenation on the N atom and all available carbon atoms except for the two sharing carbon atoms on the fused ring was observed. Spectral groupings were achieved according to their behaviors after maintenance of the matrix in darkness and on secondary photolysis at various wavelengths. The assignments were supported via comparison of the experimental results with the vibrational wavenumbers and IR intensities of possible isomers predicted using the B3LYP/6-311++G(d,p) method. The implications in the identification of the UIR band are discussed.
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Affiliation(s)
- Prasad Ramesh Joshi
- Department of Applied Chemistry and Institute of Molecular Science, National Yang Ming Chiao Tung University, Hsinchu 300093, Taiwan.
| | - Masashi Tsuge
- Institute of Low Temperature Science, Hokkaido University, Sapporo 060-0819, Japan.
| | - Chih-Yu Tseng
- Department of Applied Chemistry and Institute of Molecular Science, National Yang Ming Chiao Tung University, Hsinchu 300093, Taiwan.
| | - Yuan-Pern Lee
- Department of Applied Chemistry and Institute of Molecular Science, National Yang Ming Chiao Tung University, Hsinchu 300093, Taiwan. .,Center for Emergent Functional Matter Science, National Yang Ming Chiao Tung University, Hsinchu 300093, Taiwan.
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19
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Xu Z. Universal scaling laws and density slopes for dark matter haloes. Sci Rep 2023; 13:4165. [PMID: 36914742 DOI: 10.1038/s41598-023-31083-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Key Words] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/31/2022] [Accepted: 03/06/2023] [Indexed: 03/16/2023] Open
Abstract
Smalls scale challenges suggest some missing pieces in our current understanding of dark matter. A cascade theory for dark matter is proposed to provide extra insights, similar to the cascade phenomenon in hydrodynamic turbulence. The kinetic energy is cascaded in dark matter from small to large scales involves a constant rate [Formula: see text] ([Formula: see text]). Confirmed by N-body simulations, the energy cascade leads to a two-thirds law for kinetic energy [Formula: see text] on scale r such that [Formula: see text]. Equivalently, a four-thirds law can be established for mean halo density [Formula: see text] enclosed in the scale radius [Formula: see text] such that [Formula: see text], which was confirmed by galaxy rotation curves. Critical properties of dark matter might be obtained by identifying key constants on relevant scales. First, the largest halo scale [Formula: see text] can be determined by [Formula: see text], where [Formula: see text] is the velocity dispersion. Second, the smallest scale [Formula: see text] is dependent on the nature of dark matter. For collisionless dark matter, [Formula: see text], where [Formula: see text] is the Planck constant. An uncertainty principle for momentum and acceleration fluctuations is also postulated. For self-interacting dark matter, [Formula: see text], where [Formula: see text] is the cross-section of interaction. On halo scale, the energy cascade leads to an asymptotic density slope [Formula: see text] for fully virialized haloes with a vanishing radial flow, which might explain the nearly universal halo density. Based on the continuity equation, halo density is analytically shown to be closely dependent on the radial flow and mass accretion, such that simulated haloes can have different limiting slopes. A modified Einasto density profile is proposed accordingly.
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20
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Hillier DJ. Photoionization and Electron–Ion Recombination in Astrophysical Plasmas. Atoms 2023; 11:54. [DOI: 10.3390/atoms11030054] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/12/2023] Open
Abstract
Photoionization and its inverse, electron–ion recombination, are key processes that influence many astrophysical plasmas (and gasses), and the diagnostics that we use to analyze the plasmas. In this review we provide a brief overview of the importance of photoionization and recombination in astrophysics. We highlight how the data needed for spectral analyses, and the required accuracy, varies considerably in different astrophysical environments. We then discuss photoionization processes, highlighting resonances in their cross-sections. Next we discuss radiative recombination, and low and high temperature dielectronic recombination. The possible suppression of low temperature dielectronic recombination (LTDR) and high temperature dielectronic recombination (HTDR) due to the radiation field and high densities is discussed. Finally we discuss a few astrophysical examples to highlight photoionization and recombination processes.
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21
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Bejaoui S, Bera PP, Salama F, Lee T. Cavity Ring-Down Spectroscopy of Anthracene, 9-Methylanthracene, and 2-Methylanthracene in Supersonic Expansion. J Phys Chem A 2023; 127:2717-2730. [PMID: 36893328 DOI: 10.1021/acs.jpca.2c08994] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/11/2023]
Abstract
The S0-S1 absorption spectra of anthracene (C14H10), 9-methylanthracene (C15H12), and 2-methylanthracene (C15H12) are measured in the ultraviolet region between 330 and 375 nm (26,666 to 30,303 cm-1) with cavity ring-down spectroscopy in supersonic free-jet expansions of argon. The associated vibronic band systems and their spectroscopic assignments are discussed and compared to previous studies performed using fluorescence excitation and dispersed fluorescence techniques. Density functional theory (DFT) calculations were carried out to study the structures and evaluate the vibrational transitions of the ground and excited states. Time-dependent DFT calculations of the first electronic excited states and Franck-Condon factor calculations were carried out to assist in the assignment of the experimentally measured vibronic bands. The vibronic spectra obtained in absorption agree well with fluorescence excitation spectra in terms of peak positions but exhibit different relative band intensities. We find a very good match between experimentally obtained vibronic line positions and the peak positions of the quantum chemically calculated Franck-Condon excitation lines.
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Affiliation(s)
- Salma Bejaoui
- Bay Area Environmental Research Institute, Moffett Field, California 94035, United States.,Space Science and Astrobiology Division, NASA Ames Research Center, Mountain View, California 94035, United States
| | - Partha P Bera
- Bay Area Environmental Research Institute, Moffett Field, California 94035, United States.,Space Science and Astrobiology Division, NASA Ames Research Center, Mountain View, California 94035, United States
| | - Farid Salama
- Space Science and Astrobiology Division, NASA Ames Research Center, Mountain View, California 94035, United States
| | - Timothy Lee
- Space Science and Astrobiology Division, NASA Ames Research Center, Mountain View, California 94035, United States
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22
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Zhao Y, Chen J, Luo Z, Chang Y, Yang J, Zhang W, Wu G, Crane SW, Hansen CS, Ding H, An F, Hu X, Xie D, Ashfold MNR, Yuan K, Yang X. The vibronic state dependent predissociation of H 2S: determination of all fragmentation processes. Chem Sci 2023; 14:2501-2517. [PMID: 36908956 PMCID: PMC9993885 DOI: 10.1039/d2sc06988a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/21/2022] [Accepted: 02/09/2023] [Indexed: 02/16/2023] Open
Abstract
Photochemistry plays a significant role in shaping the chemical reaction network in the solar nebula and interstellar clouds. However, even in a simple triatomic molecule photodissociation, determination of all fragmentation processes is yet to be achieved. In this work, we present a comprehensive study of the photochemistry of H2S, derived from cutting-edge translational spectroscopy measurements of the H, S(1D) and S(1S) atom products formed by photolysis at wavelengths across the range 155-120 nm. The results provide detailed insights into the energy disposal in the SH(X), SH(A) and H2 co-fragments, and the atomisation routes leading to two H atoms along with S(3P) and S(1D) atoms. Theoretical calculations allow the dynamics of all fragmentation processes, especially the bimodal internal energy distributions in the diatomic products, to be rationalised in terms of non-adiabatic transitions between potential energy surfaces of both 1A' and 1A'' symmetry. The comprehensive picture of the wavelength-dependent (or vibronic state-dependent) photofragmentation behaviour of H2S will serve as a text-book example illustrating the importance of non-Born-Oppenheimer effects in molecular photochemistry, and the findings should be incorporated in future astrochemical modelling.
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Affiliation(s)
- Yarui Zhao
- School of Physics, Key Laboratory of Materials Modification by Laser, Ion and Electron Beams, Chinese Ministry of Education, Dalian University of Technology Dalian 116024 China.,State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China
| | - Junjie Chen
- Institute of Theoretical and Computational Chemistry, Key Laboratory of Mesoscopic Chemistry, School of Chemistry and Chemical Engineering, Nanjing University Nanjing 210023 China
| | - Zijie Luo
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China
| | - Yao Chang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China
| | - Jiayue Yang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China
| | - Weiqing Zhang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China
| | - Guorong Wu
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China
| | - Stuart W Crane
- School of Chemistry, University of Bristol Bristol BS8 1TS UK
| | | | - Hongbin Ding
- School of Physics, Key Laboratory of Materials Modification by Laser, Ion and Electron Beams, Chinese Ministry of Education, Dalian University of Technology Dalian 116024 China
| | - Feng An
- Institute of Theoretical and Computational Chemistry, Key Laboratory of Mesoscopic Chemistry, School of Chemistry and Chemical Engineering, Nanjing University Nanjing 210023 China
| | - Xixi Hu
- Kuang Yaming Honors School, Institute for Brain Sciences, Jiangsu Key Laboratory of Vehicle Emissions Control, Center of Modern Analysis, Nanjing University Nanjing 210023 China .,Hefei National Laboratory Hefei 230088 China
| | - Daiqian Xie
- Institute of Theoretical and Computational Chemistry, Key Laboratory of Mesoscopic Chemistry, School of Chemistry and Chemical Engineering, Nanjing University Nanjing 210023 China.,Hefei National Laboratory Hefei 230088 China
| | | | - Kaijun Yuan
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China .,Hefei National Laboratory Hefei 230088 China
| | - Xueming Yang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences Dalian 116023 China .,Hefei National Laboratory Hefei 230088 China.,Department of Chemistry, Southern University of Science and Technology Shenzhen 518055 China
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23
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Beylin VA, Khlopov MY, Sopin DO. Charge Asymmetry of New Stable Families in Baryon Asymmetrical Universe. Symmetry (Basel) 2023; 15:657. [DOI: 10.3390/sym15030657] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/08/2023] Open
Abstract
The new stable fermion family, with Standard Model electroweak (EW) charges, should take part in sphaleron transitions in the early Universe before breaking of the EW symmetry. The conditions of balance between the excess of new fermions (additional generation of new superheavy U, D quarks and new E, N leptons) and baryon asymmetry, were considered at temperatures above, and below, the phase transition, using a system of equations for chemical potentials.
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24
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Narayan R, Quataert E. Black holes up close. Nature 2023; 615:597-604. [PMID: 36949335 DOI: 10.1038/s41586-023-05768-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/24/2022] [Accepted: 01/27/2023] [Indexed: 03/24/2023]
Abstract
Recent developments have ushered in a new era in the field of black-hole astrophysics, providing a direct view of the remarkable environment near black-hole event horizons. These observations have enabled astronomers to confirm long-standing ideas on the physics of gas flowing into black holes with temperatures that are hundreds of times greater than at the centre of the Sun. At the same time, the observations have conclusively shown that light rays near a black hole experience large deflections that cause a dark shadow in the centre of the image, an effect predicted by Einstein's theory of general relativity. With further investment, this field is poised to deliver decades of advances in our understanding of gravity and black holes through stringent tests of general relativity, as well as insights into the role of black holes as the central engines powering a wide range of astronomical phenomena.
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Affiliation(s)
- Ramesh Narayan
- Center for Astrophysics, Harvard & Smithsonian, Cambridge, MA, USA.
- Black Hole Initiative, Harvard University, Cambridge, MA, USA.
| | - Eliot Quataert
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
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25
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Tobin JJ, van 't Hoff MLR, Leemker M, van Dishoeck EF, Paneque-Carreño T, Furuya K, Harsono D, Persson MV, Cleeves LI, Sheehan PD, Cieza L. Deuterium-enriched water ties planet-forming disks to comets and protostars. Nature 2023; 615:227-30. [PMID: 36890372 DOI: 10.1038/s41586-022-05676-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/02/2022] [Accepted: 12/21/2022] [Indexed: 03/10/2023]
Abstract
Water is a fundamental molecule in the star and planet formation process, essential for catalysing the growth of solid material and the formation of planetesimals within disks1,2. However, the water snowline and the HDO:H2O ratio within proto-planetary disks have not been well characterized because water only sublimates at roughly 160 K (ref. 3), meaning that most water is frozen out onto dust grains and that the water snowline radii are less than 10 AU (astronomical units)4,5. The sun-like protostar V883 Ori (M* = 1.3 M⊙)6 is undergoing an accretion burst7, increasing its luminosity to roughly 200 L⊙ (ref. 8), and previous observations suggested that its water snowline is 40-120 AU in radius6,9,10. Here we report the direct detection of gas phase water (HDO and [Formula: see text]) from the disk of V883 Ori. We measure a midplane water snowline radius of approximately 80 AU, comparable to the scale of the Kuiper Belt, and detect water out to a radius of roughly 160 AU. We then measure the HDO:H2O ratio of the disk to be (2.26 ± 0.63) × 10-3. This ratio is comparable to those of protostellar envelopes and comets, and exceeds that of Earth's oceans by 3.1σ. We conclude that disks directly inherit water from the star-forming cloud and this water becomes incorporated into large icy bodies, such as comets, without substantial chemical alteration.
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26
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Vincentelli FM, Neilsen J, Tetarenko AJ, Cavecchi Y, Castro Segura N, Del Palacio S, van den Eijnden J, Vasilopoulos G, Altamirano D, Armas Padilla M, Bailyn CD, Belloni T, Buisson DJK, Cúneo VA, Degenaar N, Knigge C, Long KS, Jiménez-Ibarra F, Milburn J, Muñoz Darias T, Özbey Arabacı M, Remillard R, Russell T. A shared accretion instability for black holes and neutron stars. Nature 2023; 615:45-49. [PMID: 36859580 DOI: 10.1038/s41586-022-05648-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/17/2022] [Accepted: 12/12/2022] [Indexed: 03/03/2023]
Abstract
Accretion disks around compact objects are expected to enter an unstable phase at high luminosity1. One instability may occur when the radiation pressure generated by accretion modifies the disk viscosity, resulting in the cyclic depletion and refilling of the inner disk on short timescales2. Such a scenario, however, has only been quantitatively verified for a single stellar-mass black hole3-5. Although there are hints of these cycles in a few isolated cases6-10, their apparent absence in the variable emission of most bright accreting neutron stars and black holes has been a continuing puzzle11. Here we report the presence of the same multiwavelength instability around an accreting neutron star. Moreover, we show that the variability across the electromagnetic spectrum-from radio to X-ray-of both black holes and neutron stars at high accretion rates can be explained consistently if the accretion disks are unstable, producing relativistic ejections during transitions that deplete or refill the inner disk. Such a new association allows us to identify the main physical components responsible for the fast multiwavelength variability of highly accreting compact objects.
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Affiliation(s)
- F M Vincentelli
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain.
- Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain.
- Department of Physics, Villanova University, Villanova, PA, USA.
- Department of Physics and Astronomy, University of Southampton, Southampton, UK.
| | - J Neilsen
- Department of Physics, Villanova University, Villanova, PA, USA
| | - A J Tetarenko
- Department of Physics and Astronomy, Texas Tech University, Lubbock, TX, USA
| | - Y Cavecchi
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Ciudad de México, Mexico
- Departament de Física, EEBE, Universitat Politècnica de Catalunya, Barcelona, Spain
| | - N Castro Segura
- Department of Physics and Astronomy, University of Southampton, Southampton, UK
| | - S Del Palacio
- Department of Space, Earth and Environment, Chalmers University of Technology, Gothenburg, Sweden
| | - J van den Eijnden
- Astrophysics, Department of Physics, University of Oxford, Oxford, UK
| | - G Vasilopoulos
- Department of Astronomy, Yale University, New Haven, CT, USA
- Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, Strasbourg, France
| | - D Altamirano
- Department of Physics and Astronomy, University of Southampton, Southampton, UK
| | - M Armas Padilla
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
- Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
| | - C D Bailyn
- Department of Astronomy, Yale University, New Haven, CT, USA
| | - T Belloni
- INAF - Osservatorio Astronomico di Brera, Merate, Italy
| | - D J K Buisson
- Department of Physics and Astronomy, University of Southampton, Southampton, UK
| | - V A Cúneo
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
- Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
| | - N Degenaar
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands
| | - C Knigge
- Department of Physics and Astronomy, University of Southampton, Southampton, UK
| | - K S Long
- Space Telescope Science Institute, Baltimore, MD, USA
- Eureka Scientific, Inc., Oakland, CA, USA
| | - F Jiménez-Ibarra
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
- Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
| | - J Milburn
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - T Muñoz Darias
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
- Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
| | - M Özbey Arabacı
- Department of Physics and Astronomy, University of Southampton, Southampton, UK
| | - R Remillard
- MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - T Russell
- INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Palermo, Italy
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27
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Dhal S, Paul RK. Investigation on CMB monopole and dipole using blackbody radiation inversion. Sci Rep 2023; 13:3316. [PMID: 36849496 PMCID: PMC9971209 DOI: 10.1038/s41598-023-30414-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/16/2022] [Accepted: 02/22/2023] [Indexed: 03/01/2023] Open
Abstract
The COBE/FIRAS dataset is used to calculate the Cosmic Microwave Background temperature and the uncertainty using the Blackbody Radiation Inversion (BRI) method. In this research work, the procedure is somewhat comparable to the mixing of weighted blackbodies in the case of the dipole. The temperature and its spreading for the monopole and dipole, respectively, are 2.741 ± 0.018 K and 2.748 ± 0.270 K. This dipole spreading exceeds the spreading predicted by taking relative motion into account (i.e., 3.3 × 10-3 K). The comparison of the probability distributions for the monopole spectrum, dipole spectrum, and their resultant is also displayed. It is shown that the distribution is symmetrically orientated. We estimated the µ and y-distortions by interpreting the spreading as the distortion and found that they are of the order of 10-4 and 10-5, respectively, for the monopole spectrum and 10-2 for the dipole spectrum. The paper also highlights the effectiveness of the BRI method and hints at future applications in the thermal nature of the early universe.
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Affiliation(s)
- Somita Dhal
- grid.418391.60000 0001 1015 3164Department of Physics, Birla Institute of Technology, Mesra, Ranchi, Jharkhand 835215 India
| | - R. K. Paul
- grid.418391.60000 0001 1015 3164Department of Physics, Birla Institute of Technology, Mesra, Ranchi, Jharkhand 835215 India
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Nakamura T, Matsumoto M, Amano K, Enokido Y, Zolensky ME, Mikouchi T, Genda H, Tanaka S, Zolotov MY, Kurosawa K, Wakita S, Hyodo R, Nagano H, Nakashima D, Takahashi Y, Fujioka Y, Kikuiri M, Kagawa E, Matsuoka M, Brearley AJ, Tsuchiyama A, Uesugi M, Matsuno J, Kimura Y, Sato M, Milliken RE, Tatsumi E, Sugita S, Hiroi T, Kitazato K, Brownlee D, Joswiak DJ, Takahashi M, Ninomiya K, Takahashi T, Osawa T, Terada K, Brenker FE, Tkalcec BJ, Vincze L, Brunetto R, Aléon-Toppani A, Chan QHS, Roskosz M, Viennet JC, Beck P, Alp EE, Michikami T, Nagaashi Y, Tsuji T, Ino Y, Martinez J, Han J, Dolocan A, Bodnar RJ, Tanaka M, Yoshida H, Sugiyama K, King AJ, Fukushi K, Suga H, Yamashita S, Kawai T, Inoue K, Nakato A, Noguchi T, Vilas F, Hendrix AR, Jaramillo-Correa C, Domingue DL, Dominguez G, Gainsforth Z, Engrand C, Duprat J, Russell SS, Bonato E, Ma C, Kawamoto T, Wada T, Watanabe S, Endo R, Enju S, Riu L, Rubino S, Tack P, Takeshita S, Takeichi Y, Takeuchi A, Takigawa A, Takir D, Tanigaki T, Taniguchi A, Tsukamoto K, Yagi T, Yamada S, Yamamoto K, Yamashita Y, Yasutake M, Uesugi K, Umegaki I, Chiu I, Ishizaki T, Okumura S, Palomba E, Pilorget C, Potin SM, Alasli A, Anada S, Araki Y, Sakatani N, Schultz C, Sekizawa O, Sitzman SD, Sugiura K, Sun M, Dartois E, De Pauw E, Dionnet Z, Djouadi Z, Falkenberg G, Fujita R, Fukuma T, Gearba IR, Hagiya K, Hu MY, Kato T, Kawamura T, Kimura M, Kubo MK, Langenhorst F, Lantz C, Lavina B, Lindner M, Zhao J, Vekemans B, Baklouti D, Bazi B, Borondics F, Nagasawa S, Nishiyama G, Nitta K, Mathurin J, Matsumoto T, Mitsukawa I, Miura H, Miyake A, Miyake Y, Yurimoto H, Okazaki R, Yabuta H, Naraoka H, Sakamoto K, Tachibana S, Connolly HC, Lauretta DS, Yoshitake M, Yoshikawa M, Yoshikawa K, Yoshihara K, Yokota Y, Yogata K, Yano H, Yamamoto Y, Yamamoto D, Yamada M, Yamada T, Yada T, Wada K, Usui T, Tsukizaki R, Terui F, Takeuchi H, Takei Y, Iwamae A, Soejima H, Shirai K, Shimaki Y, Senshu H, Sawada H, Saiki T, Ozaki M, Ono G, Okada T, Ogawa N, Ogawa K, Noguchi R, Noda H, Nishimura M, Namiki N, Nakazawa S, Morota T, Miyazaki A, Miura A, Mimasu Y, Matsumoto K, Kumagai K, Kouyama T, Kikuchi S, Kawahara K, Kameda S, Iwata T, Ishihara Y, Ishiguro M, Ikeda H, Hosoda S, Honda R, Honda C, Hitomi Y, Hirata N, Hirata N, Hayashi T, Hayakawa M, Hatakeda K, Furuya S, Fukai R, Fujii A, Cho Y, Arakawa M, Abe M, Watanabe S, Tsuda Y. Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples. Science 2023; 379:eabn8671. [PMID: 36137011 DOI: 10.1126/science.abn8671] [Citation(s) in RCA: 14] [Impact Index Per Article: 14.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Samples of the carbonaceous asteroid Ryugu were brought to Earth by the Hayabusa2 spacecraft. We analyzed 17 Ryugu samples measuring 1 to 8 millimeters. Carbon dioxide-bearing water inclusions are present within a pyrrhotite crystal, indicating that Ryugu's parent asteroid formed in the outer Solar System. The samples contain low abundances of materials that formed at high temperatures, such as chondrules and calcium- and aluminum-rich inclusions. The samples are rich in phyllosilicates and carbonates, which formed through aqueous alteration reactions at low temperature, high pH, and water/rock ratios of <1 (by mass). Less altered fragments contain olivine, pyroxene, amorphous silicates, calcite, and phosphide. Numerical simulations, based on the mineralogical and physical properties of the samples, indicate that Ryugu's parent body formed ~2 million years after the beginning of Solar System formation.
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Affiliation(s)
- T Nakamura
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M Matsumoto
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - K Amano
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - Y Enokido
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M E Zolensky
- NASA Johnson Space Center; Houston, TX 77058, USA
| | - T Mikouchi
- The University Museum, The University of Tokyo, Tokyo 113-0033, Japan
| | - H Genda
- Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo 152-8550, Japan
| | - S Tanaka
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - M Y Zolotov
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - K Kurosawa
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - S Wakita
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - R Hyodo
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - H Nagano
- Department of Mechanical Systems Engineering, Nagoya University, Nagoya 464-8603, Japan
| | - D Nakashima
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - Y Takahashi
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan.,Isotope Science Center, The University of Tokyo, Tokyo 113-0032, Japan
| | - Y Fujioka
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M Kikuiri
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - E Kagawa
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M Matsuoka
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Meudon 92195 France.,Geological Survey of Japan, National Institute of Advanced Industrial Science and Technology (AIST), Tsukuba, 305-8567, Japan
| | - A J Brearley
- Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM 87131, USA
| | - A Tsuchiyama
- Research Organization of Science and Technology, Ritsumeikan University, Kusatsu 525-8577, Japan.,Key Laboratory of Mineralogy and Metallogeny, Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences (CAS), Guangzhou 510640, China.,Center for Excellence in Deep Earth Science, CAS, Guangzhou 510640, China
| | - M Uesugi
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - J Matsuno
- Research Organization of Science and Technology, Ritsumeikan University, Kusatsu 525-8577, Japan
| | - Y Kimura
- Institute of Low Temperature Science, Hokkaido University, Sapporo 060-0819, Japan
| | - M Sato
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - R E Milliken
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - E Tatsumi
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan.,Instituto de Astrofísica de Canarias, University of La Laguna, Tenerife 38205, Spain
| | - S Sugita
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - T Hiroi
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - K Kitazato
- Aizu Research Center for Space Informatics, The University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - D Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195 USA
| | - D J Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195 USA
| | - M Takahashi
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - K Ninomiya
- Institute for Radiation Sciences, Osaka University, Toyonaka 560-0043, Japan
| | - T Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa 277-8583, Japan.,Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
| | - T Osawa
- Materials Sciences Research Center, Japan Atomic Energy Agency, Tokai 319-1195, Japan
| | - K Terada
- Department of Earth and Space Science, Osaka University, Toyonaka 560-0043, Japan
| | - F E Brenker
- Institute of Geoscience, Goethe University, Frankfurt, 60438 Frankfurt am Main, Germany
| | - B J Tkalcec
- Institute of Geoscience, Goethe University, Frankfurt, 60438 Frankfurt am Main, Germany
| | - L Vincze
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - R Brunetto
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - A Aléon-Toppani
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - Q H S Chan
- Department of Earth Sciences, Royal Holloway, University of London, Egham TW20 0EX, UK
| | - M Roskosz
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, Muséum National d'Histoire Naturelle, Centre national de la recherche scientifique (CNRS), Sorbonne Université, Paris, France
| | - J-C Viennet
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, Muséum National d'Histoire Naturelle, Centre national de la recherche scientifique (CNRS), Sorbonne Université, Paris, France
| | - P Beck
- Institut de Planétologie et d'Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, 38000 Grenoble, France
| | - E E Alp
- Advanced Photon Source, Argonne National Laboratory, Argonne, IL 60439, USA
| | - T Michikami
- Faculty of Engineering, Kindai University, Higashi-Hiroshima 739-2116, Japan
| | - Y Nagaashi
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan.,Department of Planetology, Kobe University, Kobe 657-8501, Japan
| | - T Tsuji
- Department of Earth Resources Engineering, Kyushu University, Fukuoka 819-0395, Japan.,School of Engineering, The University of Tokyo, Tokyo 113-0033, Japan
| | - Y Ino
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Physics, Kwansei Gakuin University, Sanda 669-1330, Japan
| | - J Martinez
- NASA Johnson Space Center; Houston, TX 77058, USA
| | - J Han
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX 77204, USA
| | - A Dolocan
- Texas Materials Institute, The University of Texas at Austin, Austin, TX 78712, USA
| | - R J Bodnar
- Department of Geoscience, Virginia Tech, Blacksburg, VA 24061, USA
| | - M Tanaka
- Materials Analysis Station, National Institute for Materials Science, Tsukuba 305-0047, Japan
| | - H Yoshida
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - K Sugiyama
- Institute for Materials Research, Tohoku University, Sendai 980-8577, Japan
| | - A J King
- Department of Earth Science, Natural History Museum, London SW7 5BD, UK
| | - K Fukushi
- Institute of Nature and Environmental Technology, Kanazawa University, Kanazawa 920-1192, Japan
| | - H Suga
- Spectroscopy Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - S Yamashita
- Department of Materials Structure Science, The Graduate University for Advanced Studies (SOKENDAI), Tsukuba, Ibaraki 305-0801, Japan.,Institute of Materials Structure Science, High-Energy Accelerator Research Organization, Tsukuba 305-0801, Japan
| | - T Kawai
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - K Inoue
- Institute of Nature and Environmental Technology, Kanazawa University, Kanazawa 920-1192, Japan
| | - A Nakato
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan.,Faculty of Arts and Science, Kyushu University, Fukuoka 819-0395, Japan
| | - F Vilas
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - A R Hendrix
- Planetary Science Institute, Tucson, AZ 85719, USA
| | | | - D L Domingue
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - G Dominguez
- Department of Physics, California State University, San Marcos, CA 92096, USA
| | - Z Gainsforth
- Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - C Engrand
- Laboratoire de Physique des 2 Infinis Irène Joliot-Curie, Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - J Duprat
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, Muséum National d'Histoire Naturelle, Centre national de la recherche scientifique (CNRS), Sorbonne Université, Paris, France
| | - S S Russell
- Department of Earth Science, Natural History Museum, London SW7 5BD, UK
| | - E Bonato
- Institute for Planetary Research, Deutsches Zentrum für Luftund Raumfahrt, Rutherfordstraße 2 12489 Berlin, Germany
| | - C Ma
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena CA 91125, USA
| | - T Kawamoto
- Department of Geosciences, Shizuoka University, Shizuoka 422-8529, Japan
| | - T Wada
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - S Watanabe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa 277-8583, Japan
| | - R Endo
- Department of Materials Science and Engineering, Tokyo Institute of Technology, Tokyo 152-8550, Japan
| | - S Enju
- Graduate School of Science and Engineering, Ehime University, Matsuyama 790-8577, Japan
| | - L Riu
- European Space Astronomy Centre, 28692 Villanueva de la Cañada, Spain
| | - S Rubino
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - P Tack
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - S Takeshita
- High Energy Accelerator Research Organization, Tokai 319-1106, Japan
| | - Y Takeichi
- Department of Materials Structure Science, The Graduate University for Advanced Studies (SOKENDAI), Tsukuba, Ibaraki 305-0801, Japan.,Institute of Materials Structure Science, High-Energy Accelerator Research Organization, Tsukuba 305-0801, Japan.,Department of Applied Physics, Osaka University, Suita 565-0871, Japan
| | - A Takeuchi
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - A Takigawa
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - D Takir
- NASA Johnson Space Center; Houston, TX 77058, USA
| | | | - A Taniguchi
- Institute for Integrated Radiation and Nuclear Science, Kyoto University, Kumatori 590-0494, Japan
| | - K Tsukamoto
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - T Yagi
- National Metrology Institute of Japan, AIST, Tsukuba 305-8565, Japan
| | - S Yamada
- Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - K Yamamoto
- Japan Fine Ceramics Center, Nagoya 456-8587, Japan
| | - Y Yamashita
- National Metrology Institute of Japan, AIST, Tsukuba 305-8565, Japan
| | - M Yasutake
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - K Uesugi
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - I Umegaki
- High Energy Accelerator Research Organization, Tokai 319-1106, Japan.,Toyota Central Research and Development Laboratories, Nagakute 480-1192, Japan
| | - I Chiu
- Institute for Radiation Sciences, Osaka University, Toyonaka 560-0043, Japan
| | - T Ishizaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - S Okumura
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome 00133, Italy
| | - C Pilorget
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France.,Institut Universitaire de France, Paris, France
| | - S M Potin
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Meudon 92195 France.,Faculty of Aerospace Engineering, Delft University of Technology, Delft, Netherlands
| | - A Alasli
- Department of Mechanical Systems Engineering, Nagoya University, Nagoya 464-8603, Japan
| | - S Anada
- Japan Fine Ceramics Center, Nagoya 456-8587, Japan
| | - Y Araki
- Department of Physical Sciences, Ritsumeikan University, Shiga 525-0058, Japan
| | - N Sakatani
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - C Schultz
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - O Sekizawa
- Spectroscopy Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - S D Sitzman
- Physical Sciences Laboratory, The Aerospace Corporation, CA 90245, USA
| | - K Sugiura
- Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo 152-8550, Japan
| | - M Sun
- Key Laboratory of Mineralogy and Metallogeny, Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences (CAS), Guangzhou 510640, China.,Center for Excellence in Deep Earth Science, CAS, Guangzhou 510640, China.,University of Chinese Academy of Sciences, Beijing 100049, China
| | - E Dartois
- Institut des Sciences Moléculaires d'Orsay, Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - E De Pauw
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - Z Dionnet
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - Z Djouadi
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - G Falkenberg
- Deutsches Elektronen-Synchrotron Photon Science, 22603 Hamburg, Germany
| | - R Fujita
- Department of Mechanical Systems Engineering, Nagoya University, Nagoya 464-8603, Japan
| | - T Fukuma
- Nano Life Science Institute, Kanazawa University, Kanazawa 920-1192, Japan
| | - I R Gearba
- Texas Materials Institute, The University of Texas at Austin, Austin, TX 78712, USA
| | - K Hagiya
- Graduate School of Life Science, University of Hyogo, Hyogo 678-1297, Japan
| | - M Y Hu
- Advanced Photon Source, Argonne National Laboratory, Argonne, IL 60439, USA
| | - T Kato
- Japan Fine Ceramics Center, Nagoya 456-8587, Japan
| | - T Kawamura
- Institut de Physique du Globe de Paris, Université de Paris, Paris 75205, France
| | - M Kimura
- Department of Materials Structure Science, The Graduate University for Advanced Studies (SOKENDAI), Tsukuba, Ibaraki 305-0801, Japan.,Institute of Materials Structure Science, High-Energy Accelerator Research Organization, Tsukuba 305-0801, Japan
| | - M K Kubo
- Division of Natural Sciences, International Christian University, Mitaka 181-8585, Japan
| | - F Langenhorst
- Institute of Geosciences, Friedrich-Schiller-Universität Jena, 07745 Jena, Germany
| | - C Lantz
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - B Lavina
- Center for Advanced Radiation Sources, University of Chicago, Chicago, IL 60637, USA
| | - M Lindner
- Institute of Geoscience, Goethe University, Frankfurt, 60438 Frankfurt am Main, Germany
| | - J Zhao
- Advanced Photon Source, Argonne National Laboratory, Argonne, IL 60439, USA
| | - B Vekemans
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - D Baklouti
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - B Bazi
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - F Borondics
- Optimized Light Source of Intermediate Energy to LURE (SOLEIL) L'Orme des Merisiers, Gif sur Yvette F-91192, France
| | - S Nagasawa
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa 277-8583, Japan.,Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
| | - G Nishiyama
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - K Nitta
- Spectroscopy Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - J Mathurin
- Institut Chimie Physique, Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - T Matsumoto
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - I Mitsukawa
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - H Miura
- Graduate School of Science, Nagoya City University, Nagoya 467-8501, Japan
| | - A Miyake
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Y Miyake
- High Energy Accelerator Research Organization, Tokai 319-1106, Japan
| | - H Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 060-0810, Japan
| | - R Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - H Yabuta
- Graduate School of Advanced Science and Engineering, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - H Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - K Sakamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - S Tachibana
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - H C Connolly
- Department of Geology, Rowan University, Glassboro, NJ 08028, USA
| | - D S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - M Yoshitake
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - K Yoshikawa
- Research and Development Directorate, JAXA, Sagamihara 252-5210, Japan
| | - K Yoshihara
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Yokota
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Yogata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - H Yano
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - Y Yamamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - D Yamamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Yamada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - T Yamada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Yada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Wada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - T Usui
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - R Tsukizaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - F Terui
- Department of Mechanical Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - H Takeuchi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - Y Takei
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - A Iwamae
- Marine Works Japan, Yokosuka 237-0063, Japan
| | - H Soejima
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - K Shirai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Shimaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - H Senshu
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - H Sawada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Ozaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - G Ono
- Research and Development Directorate, JAXA, Sagamihara 252-5210, Japan
| | - T Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Chemistry, The University of Tokyo, Tokyo 113-0033, Japan
| | - N Ogawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Ogawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - R Noguchi
- Faculty of Science, Niigata University, Niigata 950-2181, Japan
| | - H Noda
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - M Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - N Namiki
- Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan.,National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - S Nakazawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Morota
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - A Miyazaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - A Miura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Mimasu
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Matsumoto
- Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan.,National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - K Kumagai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - T Kouyama
- Digital Architecture Research Center, National Institute of Advanced Industrial Science and Technology, Tokyo 135-0064, Japan
| | - S Kikuchi
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan.,National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - K Kawahara
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - S Kameda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - T Iwata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - Y Ishihara
- JAXA Space Exploration Center, JAXA, Sagamihara 252-5210, Japan
| | - M Ishiguro
- Department of Physics and Astronomy, Seoul National University, Seoul 08826, Korea
| | - H Ikeda
- Research and Development Directorate, JAXA, Sagamihara 252-5210, Japan
| | - S Hosoda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - R Honda
- Department of Information Science, Kochi University, Kochi 780-8520, Japan.,Center for Data Science, Ehime University, Matsuyama 790-8577, Japan
| | - C Honda
- Aizu Research Center for Space Informatics, The University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Y Hitomi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - N Hirata
- Department of Planetology, Kobe University, Kobe 657-8501, Japan
| | - N Hirata
- Aizu Research Center for Space Informatics, The University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - T Hayashi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Hayakawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Hatakeda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - S Furuya
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - R Fukai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - A Fujii
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Cho
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - M Arakawa
- Department of Planetology, Kobe University, Kobe 657-8501, Japan
| | - M Abe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - S Watanabe
- Department of Earth and Environmental Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Y Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
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29
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Spaniol JT, Lee KLK, Pirali O, Puzzarini C, Martin-Drumel MA. A rotational investigation of the three isomeric forms of cyanoethynylbenzene (HCC-C 6H 4-CN): benchmarking experiments and calculations using the "Lego brick" approach. Phys Chem Chem Phys 2023; 25:6397-6405. [PMID: 36779600 DOI: 10.1039/d2cp04825f] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
We report the study of three structural isomers of phenylpropiolonitrile (3-phenyl-2-propynenitrile, C6H5-C3N) containing an alkyne function and a cyano group, namely ortho-, meta-, and para-cyanoethynylbenzene (HCC-C6H4-CN). The pure rotational spectra of these species have been recorded at room temperature in the millimeter-wave domain using a chirped-pulse spectrometer (75-110 GHz) and a source-frequency modulation spectrometer (140-220 GHz). Assignments of transitions in the vibrational ground state and several vibrationally excited states were supported by quantum chemical calculations using the so-called "Lego brick" approach [A. Melli, F. Tonolo, V. Barone and C. Puzzarini, J. Phys. Chem. A, 2021, 125, 9904-9916]. From these assignments, accurate spectroscopic (rotational and centrifugal distortion) constants have been derived: for all species and all observed vibrational states, predicted rotational constants show relative accuracy better than 0.1%, and often of the order of 0.01%, compared to the experimental values. The present work hence further validates the use of the "Lego brick" approach for predicting spectroscopic constants with high precision.
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Affiliation(s)
- Jean-Thibaut Spaniol
- Université Paris-Saclay, CNRS, Institut des Sciences Moléculaires d'Orsay, 91405 Orsay, France.
| | - Kin Long Kelvin Lee
- Intel Accelerated Computing Systems and Graphics Group, Intel JF5 2111 NE 25th Ave, Hillsboro, OR 97124, USA
| | - Olivier Pirali
- Université Paris-Saclay, CNRS, Institut des Sciences Moléculaires d'Orsay, 91405 Orsay, France.
| | - Cristina Puzzarini
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, via F. Selmi 2, 40126 Bologna, Italy.
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30
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Vysotskii VI, Vysotskyy MV. Self-Controlled Flashing Nuclear Fusion in Stationary Magnetized Low-Temperature Plasma. Fusion Science and Technology 2023. [DOI: 10.1080/15361055.2022.2151284] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/23/2023]
Affiliation(s)
- V. I. Vysotskii
- Taras Shevchenko National University of Kyiv, 64/13, Volodymyrska Street, Kyiv, 01601, Ukraine
| | - M. V. Vysotskyy
- Taras Shevchenko National University of Kyiv, 64/13, Volodymyrska Street, Kyiv, 01601, Ukraine
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31
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Mandt KE. The first dedicated ice giants mission. Science 2023; 379:640-642. [PMID: 36795812 DOI: 10.1126/science.ade8446] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/18/2023]
Abstract
The mysteries of the Uranus system can be unlocked through interdisciplinary exploration.
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32
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Zhang C, Turner AM, Wang J, Marks JH, Fortenberry RC, Kaiser RI. Low-Temperature Thermal Formation of the Cyclic Methylphosphonic Acid Trimer [c-(CH 3 PO 2 ) 3 ]. Chemphyschem 2023; 24:e202200660. [PMID: 36283955 DOI: 10.1002/cphc.202200660] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/31/2022] [Revised: 10/22/2022] [Indexed: 11/11/2022]
Abstract
We report the formation of the cyclic methylphosphonic acid trimer [c-(CH3 PO2 )3 ] through condensation reactions during thermal processing of low-temperature methylphosphonic acid samples exploiting photoionization reflectron time-of-flight mass spectrometry (PI-ReTOF-MS) along with electronic structure calculations. Cyclic methylphosphonic acid trimers are formed in the solid state and detected together with its protonated species in the gas phase upon single photon ionization. Our studies provide an understanding of the preparation of phosphorus-bearing potentially prebiotic molecules and the fundamental knowledge of low-temperature phosphorus chemistry in extraterrestrial environments.
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Affiliation(s)
- Chaojiang Zhang
- Department of Chemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI 96822, USA.,W. M. Keck Laboratory in Astrochemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI, 96822, USA
| | - Andrew M Turner
- Department of Chemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI 96822, USA.,W. M. Keck Laboratory in Astrochemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI, 96822, USA
| | - Jia Wang
- Department of Chemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI 96822, USA.,W. M. Keck Laboratory in Astrochemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI, 96822, USA
| | - Joshua H Marks
- Department of Chemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI 96822, USA.,W. M. Keck Laboratory in Astrochemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI, 96822, USA
| | - Ryan C Fortenberry
- Department of Chemistry & Biochemistry, University of Mississippi, Oxford, Mississippi, MS, 38677, USA
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI 96822, USA.,W. M. Keck Laboratory in Astrochemistry, University of Hawaii at Manoa, 2545 McCarthy Mall, Honolulu, HI, 96822, USA
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33
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Nath G. Analytical Solution for Unsteady Adiabatic Flow Behind the Blast Wave in a Non-ideal Gas and Small Inert Solid Particles Mixture. Proc Natl Acad Sci , India, Sect A Phys Sci 2023. [DOI: 10.1007/s40010-023-00811-5] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/15/2023]
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34
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Mou G, Sun D, Fang T, Wang W, Zhang R, Yuan F, Sofue Y, Wang T, He Z. Asymmetric eROSITA bubbles as the evidence of a circumgalactic medium wind. Nat Commun 2023; 14:781. [PMID: 36774356 DOI: 10.1038/s41467-023-36478-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Key Words] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/28/2022] [Accepted: 01/31/2023] [Indexed: 02/13/2023] Open
Abstract
The eROSITA bubbles are detected via the instrument with the same name. The northern bubble shows noticeable asymmetric features, including distortion to the west and enhancement in the eastern edge, while the southern counterpart is significantly dimmer. Their origins are debated. Here, we performed hydrodynamic simulations showing that asymmetric eROSITA bubbles favor a dynamic, circumgalactic medium wind model, but disfavor other mechanisms such as a non-axisymmetric halo gas or a tilted nuclear outflow. The wind from the east by north direction in Galactic coordinates blows across the northern halo with a velocity of about 200 km s-1, and part of it enters the southern halo. This creates a dynamic halo medium and redistributes both density and metallicity within. This naturally explains the asymmetric bubbles in both the morphology and surface brightness. Our results suggest that our Galaxy is accreting low-abundance circumgalactic medium from one side while providing outflow feedback.
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35
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Yan S, Zhang R, Zhang S, Ma X. Methane Cluster Fragmentation by Fast Electron Impact. Atoms 2023; 11:35. [DOI: 10.3390/atoms11020035] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/12/2023] Open
Abstract
We investigate the fragmentation of the CH4 cluster by fast electron impact at stagnation pressures from 0.5 bar to 16 bar. By measuring the time of flight spectrum (TOF), two types of ions, including (CH4)n−1CH5+ and (CH4)n−2(C2Hm)+, are observed. In the 1D TOF spectrum, it is shown that for the stagnation pressure larger than 4 bar, the former ion is predominant for each n, similar to the previous experimental result. However, as the pressure decreases to 0.5 or 2 bar, the contribution of the C2Hm+ ion is dominant over that of the CH4CH5+ ion. In the 2D coincident TOF spectrum, the above two patterns of ions are also distinguished, and the enhancement of C2Hm+ is observed at 4 bar pressure. The phenomena appearing in 2D and 1D TOF spectra imply that the C2Hm+ ion prefers to survive in a smaller cluster, while the stabilization of the protonated ion needs a more massive cluster environment.
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36
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Kibaroğlu S, Cebecioğlu O, Saban A. Gauging the Maxwell Extended GLn,R and SLn+1,R Algebras. Symmetry (Basel) 2023; 15:464. [DOI: 10.3390/sym15020464] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/11/2023] Open
Abstract
We consider the extension of the general-linear and special-linear algebras by employing the Maxwell symmetry in D space-time dimensions. We show how various Maxwell extensions of the ordinary space-time algebras can be obtained by a suitable contraction of generalized algebras. The extended Lie algebras could be useful in the construction of generalized gravity theories and the objects that couple to them. We also consider the gravitational dynamics of these algebras in the framework of the gauge theories of gravity. By adopting the symmetry-breaking mechanism of the Stelle–West model, we present some modified gravity models that contain the generalized cosmological constant term in four dimensions.
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37
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Marlton SJP, Buntine JT, Watkins P, Liu C, Jacovella U, Carrascosa E, Bull JN, Bieske EJ. Probing Colossal Carbon Rings. J Phys Chem A 2023; 127:1168-1178. [PMID: 36703560 DOI: 10.1021/acs.jpca.2c07068] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/28/2023]
Abstract
Carbon aggregates containing between 10 and 30 atoms preferentially arrange themselves as planar rings. To learn more about this exotic allotrope of carbon, electronic spectra are measured for even cyclo[n]carbon radical cations (C14+-C36+) using two-color photodissociation action spectroscopy. To eliminate spectral contributions from other isomers, the target cyclo[n]carbon radical cations are isomer-selected using a drift tube ion mobility spectrometer prior to spectroscopic interrogation. The electronic spectra exhibit sharp transitions spanning the visible and near-infrared spectral regions with the main absorption band shifting progressively to longer wavelength by ≈100 nm for every additional two carbon atoms. This behavior is rationalized with a Hückel theory model describing the energies of the in-plane and out-of-plane π orbitals. Photoexcitation of smaller carbon rings leads preferentially to neutral C3 and C5 loss, whereas rings larger than C24+ tend to also decompose into two smaller rings, which, when possible, have aromatic stability. Generally, the observed charged photofragments correspond to low energy fragment pairs, as predicted by density functional theory calculations (CAM-B3LYP-D3(BJ)/cc-pVDZ). Using action spectroscopy it is confirmed that C14+ and C18+ photofragments from C28+ rings have cyclic structures.
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Affiliation(s)
- Samuel J P Marlton
- School of Chemistry, The University of Melbourne, Victoria, Australia3010
| | - Jack T Buntine
- School of Chemistry, The University of Melbourne, Victoria, Australia3010
| | - Patrick Watkins
- School of Chemistry, The University of Melbourne, Victoria, Australia3010
| | - Chang Liu
- School of Chemistry, The University of Melbourne, Victoria, Australia3010
| | - Ugo Jacovella
- Université Paris-Saclay, CNRS, Institut des Sciences Moléculaires d'Orsay, 91405Orsay, France
| | - Eduardo Carrascosa
- Bruker Daltonics GmbH & Co. KG, Fahrenheitstrasse 4, 28359Bremen, Germany
| | - James N Bull
- School of Chemistry, Norwich Research Park, University of East Anglia, NorwichNR4 7TJ, United Kingdom
| | - Evan J Bieske
- School of Chemistry, The University of Melbourne, Victoria, Australia3010
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38
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He J, Pérez Rickert PC, Suhasaria T, Sohier O, Bäcker T, Demertzi D, Vidali G, Henning TK. New measurement of the diffusion of carbon dioxide on non-porous amorphous solid water. Mol Phys 2023. [DOI: 10.1080/00268976.2023.2176181] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/11/2023]
Affiliation(s)
- Jiao He
- Max Planck Institute for Astronomy, Heidelberg, Germany
| | - Paula Caroline Pérez Rickert
- Max Planck Institute for Astronomy, Heidelberg, Germany
- Department for Physics and Astronomy, Heidelberg University, Heidelberg, Germany
| | | | - Orianne Sohier
- Max Planck Institute for Astronomy, Heidelberg, Germany
- Département de chimie, École normale supérieure, PSL University, Paris, France
| | - Tia Bäcker
- Max Planck Institute for Astronomy, Heidelberg, Germany
- Physics Department, University of Helsinki, Helsinki, Finland
| | - Dimitra Demertzi
- Max Planck Institute for Astronomy, Heidelberg, Germany
- Institute for Molecules and Materials, Radboud University, Nijmegen, Netherlands
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39
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Zhelyazkova V, Martins FBV, Schilling S, Merkt F. Reaction of an Ion and a Free Radical near 0 K: He + + NO → He + N + + O. J Phys Chem A 2023; 127:1458-1468. [PMID: 36752385 PMCID: PMC9940198 DOI: 10.1021/acs.jpca.2c08221] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/09/2023]
Abstract
The reactions between ions and free radicals are among the fastest chemical reactions. They are predicted to proceed with large rates, even near 0 K, but so far, this prediction has not been verified experimentally. We report on measurements of the rate coefficient of the reaction between the ion He+ and the free radical NO at collision energies in the range between 0 and ∼ kB·10 K. To avoid heating of the ions by stray electric fields, the reaction is observed within the large orbit of a Rydberg electron of principal quantum number n ≥ 30, which shields the ion from external electric fields without affecting the reaction. Low collision energies are reached by merging a supersonic beam of He Rydberg atoms with a supersonic beam of NO molecules and adjusting their relative velocity using a chip-based Rydberg-Stark decelerator and deflector. We observe a strong enhancement of the reaction rate at collision energies below ∼kB·2 K. This enhancement is interpreted on the basis of adiabatic-channel capture-rate calculations as arising from the near-degenerate rotational levels of opposite parity resulting from the Λ-doubling in the X 2Π1/2 ground state of NO. With these new results, we examine the reliability of broadly used approximate analytic expressions for the thermal rate constants of ion-molecule reactions at low temperatures.
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40
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Abid A, Veteläinen O, Boudjemia N, Pelimanni E, Kivimäki A, Alatalo M, Huttula M, Björneholm O, Patanen M. Forming Bonds While Breaking Old Ones: Isomer-Dependent Formation of H 3O + from Aminobenzoic Acid During X-ray-Induced Fragmentation. J Phys Chem A 2023; 127:1395-1401. [PMID: 36749682 PMCID: PMC9940210 DOI: 10.1021/acs.jpca.2c06869] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/08/2023]
Abstract
Intramolecular hydrogen transfer, a reaction where donor and acceptor sites of a hydrogen atom are part of the same molecule, is a ubiquitous reaction in biochemistry and organic synthesis. In this work, we report hydronium ion (H3O+) production from aminobenzoic acid (ABA) after core-level ionization with soft X-ray synchrotron radiation. The formation of H3O+ during the fragmentation requires that at least two hydrogen atoms migrate to one of the oxygen atoms within the molecule. The comparison of two structural isomers, ortho- and meta-ABA, revealed that the production of H3O+ depends strongly on the structure of the molecule, the ortho-isomer being much more prone to produce H3O+. The isomer-dependency suggests that the amine group acts as a donor in the hydrogen transfer process. In the case of ortho-ABA, detailed H3O+ production pathways were investigated using photoelectron-photoion-photoion coincidence (PEPIPICO) spectroscopy. It was found that H3O+ can result from a direct two-body dissociation but also from sequential fragmentation processes.
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