151
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Colley JE, Orr DS, Duncan MA. Electronic Transition of the l-C6+ Cation at 417 nm. J Chem Phys 2022; 157:121102. [DOI: 10.1063/5.0106183] [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: 11/15/2022] Open
Abstract
A new electronic transition is reported for the linear C6+ cation with an origin at 416.8 nm. This spectrum can be compared to the matrix isolation spectra at lower energies reported previously by Fulara et al. (J. Chem. Phys. 123, 044305 (2005)), which assigned linear and cyclic isomers, and to the gas phase spectrum reported previously by Campbell and Dunk (Rev. Sci. Instrum. 90, 103101 (2019)), which detected the same cyclic-isomer spectrum reported by Fulara. Comparisons to electronically excited states and vibrations predicted by various forms of theory allow assignment of the spectrum to a new electronic state of linear C6+. The spectrum consists of a strong origin band, two vibronic progression members at higher energy and four hotbands at lower energies. The hotbands provide the first gas phase information on ground state vibrational frequencies. The vibronic structure of this excited state of C6+ provides a severe challenge to computational chemistry.
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Affiliation(s)
| | | | - Michael A. Duncan
- Department of Chemistry, University of Georgia, United States of America
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152
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Guan Y, Kosowsky A. Distinguishing primordial magnetic fields from inflationary tensor perturbations in the cosmic microwave background. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.063505] [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: 11/07/2022]
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153
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Hattori K, Hongo M, Huang X. New Developments in Relativistic Magnetohydrodynamics. Symmetry (Basel) 2022; 14:1851. [DOI: 10.3390/sym14091851] [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: 11/16/2022] Open
Abstract
Relativistic magnetohydrodynamics (RMHD) provides an extremely useful description of the low-energy long-wavelength phenomena in a variety of physical systems from quark–gluon plasma in heavy-ion collisions to matters in supernova, compact stars, and early universe. We review the recent theoretical progresses of RMHD, such as a formulation of RMHD from the perspective of magnetic flux conservation using the entropy–current analysis, the nonequilibrium statistical operator approach applied to quantum electrodynamics, and the relativistic kinetic theory. We discuss how the transport coefficients in RMHD are computed in kinetic theory and perturbative quantum field theories. We also explore the collective modes and instabilities in RMHD with a special emphasis on the role of chirality in a parity-odd plasma. We also give some future prospects of RMHD, including the interaction with spin hydrodynamics and the new kinetic framework with magnetic flux conservation.
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154
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Abstract
The original Friedmann (1922) and Lemaitre (1927) cosmological model corresponds to a classical solution of General Relativity (GR), with the same uniform (FLRW) metric as the standard cosmology, but bounded to a sphere of radius R and empty space outside. We study the junction conditions for R to show that a co-moving observer, like us, located anywhere inside R, measures the same background and has the same past light-cone as an observer in an infinite FLRW with the same density. We also estimate the mass M inside R and show that in the observed universe R<rS≡2 GM, which corresponds to a Black Hole Universe (BHU). We argue that this original Friedmann–Lemaitre model can explain the observed cosmic acceleration without the need of Dark Energy, because rS acts like a cosmological constant Λ=3/rS2. The same solution can describe the interior of a stellar or galactic BHs. In co-moving coordinates the BHU is expanding while in physical or proper coordinates it is asymptotically static. Such frame duality corresponds to a simple Lorentz transformation. The BHU therefore provides a physical BH solution with an asymptotically deSitter metric interior that merges into a Schwarzschild metric exterior without discontinuities.
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155
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Dai N, Gong Y, Jiang T, Liang D. Intermediate mass-ratio inspirals with dark matter minispikes. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.064003] [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: 11/07/2022]
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156
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Graham HV, Elsila JE, Dworkin JP, Sandford SA, Aponte JC. Deuterium Isotope Fractionation of Polycyclic Aromatic Hydrocarbons in Meteorites as an Indicator of Interstellar/Protosolar Processing History. Life (Basel) 2022; 12:life12091368. [PMID: 36143402 PMCID: PMC9502081 DOI: 10.3390/life12091368] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/10/2022] [Revised: 08/01/2022] [Accepted: 08/02/2022] [Indexed: 11/16/2022] Open
Abstract
The stable isotope composition of soluble and insoluble organic compounds in carbonaceous chondrites can be used to determine the provenance of organic molecules in space. Deuterium enrichment in meteoritic organics could be a residual signal of synthetic reactions occurring in the cold interstellar medium or an indicator of hydrothermal parent-body reactions. δD values have been measured in grains and bulk samples for a wide range of meteorites; however, these reservoirs are highly variable and may have experienced fractionation during thermal and/or aqueous alteration. Among the plethora of organic compounds in meteorites are polycyclic aromatic hydrocarbons (PAHs), which are stable and abundant in carbonaceous chondrites, and their δD ratio may preserve evidence about their formation environment as well as the influence of parent-body processes. This study tests hypotheses about the potential links between PAHs-deuteration concentrations and their formation conditions by examining the δD ratio of PAHs in three CM carbonaceous chondrites representing an aqueous alteration gradient. We use deuterium enrichments in soluble 2–5-ring PAHs as an indicator of either photon-driven deuteration due to unimolecular photodissociation in warm regions of space, gas-phase ion–molecule reactions in cold interstellar regions of space, or UV photolysis in ices. We also test hypothesized reaction pathways during parent-body processing that differ between partially and fully aromatized PAHs. New methodological approaches were developed to extract small, volatile PAHs without fractionation. Our results suggest that meteoritic PAHs could have formed through reactions in cold regions, with possible overprinting of deuterium enrichment during aqueous parent-body alteration, but the data could not rule out PAH alteration in icy mantles as well.
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Affiliation(s)
- Heather V. Graham
- Solar System Exploration Division, NASA Goddard Space Flight Center, MS-691, Greenbelt, MD 20771, USA
- Correspondence:
| | - Jamie E. Elsila
- Solar System Exploration Division, NASA Goddard Space Flight Center, MS-691, Greenbelt, MD 20771, USA
| | - Jason P. Dworkin
- Solar System Exploration Division, NASA Goddard Space Flight Center, MS-691, Greenbelt, MD 20771, USA
| | - Scott A. Sandford
- Space Science and Astrobiology Division, NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035, USA
| | - Jose C. Aponte
- Solar System Exploration Division, NASA Goddard Space Flight Center, MS-691, Greenbelt, MD 20771, USA
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157
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Xu H, Niu JR, Chen P, Lee KJ, Zhu WW, Dong S, Zhang B, Jiang JC, Wang BJ, Xu JW, Zhang CF, Fu H, Filippenko AV, Peng EW, Zhou DJ, Zhang YK, Wang P, Feng Y, Li Y, Brink TG, Li DZ, Lu W, Yang YP, Caballero RN, Cai C, Chen MZ, Dai ZG, Djorgovski SG, Esamdin A, Gan HQ, Guhathakurta P, Han JL, Hao LF, Huang YX, Jiang P, Li CK, Li D, Li H, Li XQ, Li ZX, Liu ZY, Luo R, Men YP, Niu CH, Peng WX, Qian L, Song LM, Stern D, Stockton A, Sun JH, Wang FY, Wang M, Wang N, Wang WY, Wu XF, Xiao S, Xiong SL, Xu YH, Xu RX, Yang J, Yang X, Yao R, Yi QB, Yue YL, Yu DJ, Yu WF, Yuan JP, Zhang BB, Zhang SB, Zhang SN, Zhao Y, Zheng WK, Zhu Y, Zou JH. A fast radio burst source at a complex magnetized site in a barred galaxy. Nature 2022; 609:685-8. [PMID: 36131036 DOI: 10.1038/s41586-022-05071-8] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/07/2021] [Accepted: 07/05/2022] [Indexed: 11/08/2022]
Abstract
Fast radio bursts (FRBs) are highly dispersed, millisecond-duration radio bursts1-3. Recent observations of a Galactic FRB4-8 suggest that at least some FRBs originate from magnetars, but the origin of cosmological FRBs is still not settled. Here we report the detection of 1,863 bursts in 82 h over 54 days from the repeating source FRB 20201124A (ref. 9). These observations show irregular short-time variation of the Faraday rotation measure (RM), which scrutinizes the density-weighted line-of-sight magnetic field strength, of individual bursts during the first 36 days, followed by a constant RM. We detected circular polarization in more than half of the burst sample, including one burst reaching a high fractional circular polarization of 75%. Oscillations in fractional linear and circular polarizations, as well as polarization angle as a function of wavelength, were detected. All of these features provide evidence for a complicated, dynamically evolving, magnetized immediate environment within about an astronomical unit (AU; Earth-Sun distance) of the source. Our optical observations of its Milky-Way-sized, metal-rich host galaxy10-12 show a barred spiral, with the FRB source residing in a low-stellar-density interarm region at an intermediate galactocentric distance. This environment is inconsistent with a young magnetar engine formed during an extreme explosion of a massive star that resulted in a long gamma-ray burst or superluminous supernova.
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158
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Jorstad SG, Marscher AP, Raiteri CM, Villata M, Weaver ZR, Zhang H, Dong L, Gómez JL, Perel MV, Savchenko SS, Larionov VM, Carosati D, Chen WP, Kurtanidze OM, Marchini A, Matsumoto K, Mortari F, Aceti P, Acosta-Pulido JA, Andreeva T, Apolonio G, Arena C, Arkharov A, Bachev R, Banfi M, Bonnoli G, Borman GA, Bozhilov V, Carnerero MI, Damljanovic G, Ehgamberdiev SA, Elsässer D, Frasca A, Gabellini D, Grishina TS, Gupta AC, Hagen-Thorn VA, Hallum MK, Hart M, Hasuda K, Hemrich F, Hsiao HY, Ibryamov S, Irsmambetova TR, Ivanov DV, Joner MD, Kimeridze GN, Klimanov SA, Knött J, Kopatskaya EN, Kurtanidze SO, Kurtenkov A, Kuutma T, Larionova EG, Leonini S, Lin HC, Lorey C, Mannheim K, Marino G, Minev M, Mirzaqulov DO, Morozova DA, Nikiforova AA, Nikolashvili MG, Ovcharov E, Papini R, Pursimo T, Rahimov I, Reinhart D, Sakamoto T, Salvaggio F, Semkov E, Shakhovskoy DN, Sigua LA, Steineke R, Stojanovic M, Strigachev A, Troitskaya YV, Troitskiy IS, Tsai A, Valcheva A, Vasilyev AA, Vince O, Waller L, Zaharieva E, Chatterjee R. Rapid quasi-periodic oscillations in the relativistic jet of BL Lacertae. Nature 2022; 609:265-268. [PMID: 36071186 DOI: 10.1038/s41586-022-05038-9] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/29/2022] [Accepted: 06/28/2022] [Indexed: 12/24/2022]
Abstract
Blazars are active galactic nuclei (AGN) with relativistic jets whose non-thermal radiation is extremely variable on various timescales1-3. This variability seems mostly random, although some quasi-periodic oscillations (QPOs), implying systematic processes, have been reported in blazars and other AGN. QPOs with timescales of days or hours are especially rare4 in AGN and their nature is highly debated, explained by emitting plasma moving helically inside the jet5, plasma instabilities6,7 or orbital motion in an accretion disc7,8. Here we report results of intense optical and γ-ray flux monitoring of BL Lacertae (BL Lac) during a dramatic outburst in 2020 (ref. 9). BL Lac, the prototype of a subclass of blazars10, is powered by a 1.7 × 108 MSun (ref. 11) black hole in an elliptical galaxy (distance = 313 megaparsecs (ref. 12)). Our observations show QPOs of optical flux and linear polarization, and γ-ray flux, with cycles as short as approximately 13 h during the highest state of the outburst. The QPO properties match the expectations of current-driven kink instabilities6 near a recollimation shock about 5 parsecs (pc) from the black hole in the wake of an apparent superluminal feature moving down the jet. Such a kink is apparent in a microwave Very Long Baseline Array (VLBA) image.
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Affiliation(s)
- S G Jorstad
- Institute for Astrophysical Research, Boston University, Boston, MA, USA. .,Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.
| | - A P Marscher
- Institute for Astrophysical Research, Boston University, Boston, MA, USA
| | - C M Raiteri
- INAF, Osservatorio Astrofisico di Torino, Torino, Italy
| | - M Villata
- INAF, Osservatorio Astrofisico di Torino, Torino, Italy
| | - Z R Weaver
- Institute for Astrophysical Research, Boston University, Boston, MA, USA
| | - H Zhang
- NASA Postdoctoral Program Fellow, Greenbelt, MD, USA.,NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - L Dong
- Department of Physics, Purdue University, West Lafayette, IN, USA
| | - J L Gómez
- Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
| | - M V Perel
- St. Petersburg State University, St. Petersburg, Russia
| | - S S Savchenko
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.,Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, Russia.,Pulkovo Observatory, St. Petersburg, Russia
| | - V M Larionov
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.,Pulkovo Observatory, St. Petersburg, Russia
| | - D Carosati
- EPT Observatories, Tijarafe, La Palma, Spain.,INAF, TNG Fundación Galileo Galilei, La Palma, Spain
| | - W P Chen
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - O M Kurtanidze
- Abastumani Observatory, Mt. Kanobili, Abastumani, Georgia.,Engelhardt Astronomical Observatory, Kazan Federal University, Tatarstan, Russia.,Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Heidelberg, Germany
| | - A Marchini
- Astronomical Observatory, Department of Physical Sciences, Earth and Environment, University of Siena, Siena, Italy
| | - K Matsumoto
- Astronomical Institute, Osaka Kyoiku University, Kashiwara, Japan
| | | | - P Aceti
- Osservatorio Astronomico Città di Seveso, Seveso, Italy.,Department of Aerospace Science and Technology, Politecnico di Milano, Milano, Italy
| | - J A Acosta-Pulido
- Instituto de Astrofísica de Canarias and Dpto. de Astrofísica, Universidad de La Laguna, Tenerife, Spain
| | - T Andreeva
- Institute of Applied Astronomy, Russian Academy of Sciences, St. Petersburg, Russia
| | - G Apolonio
- Department of Physics and Astronomy, Brigham Young University, Provo, UT, USA
| | - C Arena
- Gruppo Astrofili Catanesi (GAC), Catania, Italy
| | - A Arkharov
- Pulkovo Observatory, St. Petersburg, Russia
| | - R Bachev
- Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria
| | - M Banfi
- Osservatorio Astronomico Città di Seveso, Seveso, Italy
| | - G Bonnoli
- Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain.,Astronomical Observatory, Department of Physical Sciences, Earth and Environment, University of Siena, Siena, Italy.,INAF-Osservatorio Astronomico di Brera, Merate, Italy
| | - G A Borman
- Crimean Astrophysical Observatory RAS, Bakhchisaray, Crimea
| | - V Bozhilov
- Department of Astronomy, Faculty of Physics, University of Sofia, Sofia, Bulgaria
| | - M I Carnerero
- INAF, Osservatorio Astrofisico di Torino, Torino, Italy
| | | | - S A Ehgamberdiev
- Ulugh Beg Astronomical Institute, Tashkent, Uzbekistan.,National University of Uzbekistan, Tashkent, Uzbekistan
| | - D Elsässer
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany.,Department of Physics, TU Dortmund University, Dortmund, Germany
| | - A Frasca
- INAF-Osservatorio Astrofisico di Catania, Catania, Italy
| | | | - T S Grishina
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - A C Gupta
- Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India
| | - V A Hagen-Thorn
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - M K Hallum
- Institute for Astrophysical Research, Boston University, Boston, MA, USA
| | - M Hart
- Institute for Astrophysical Research, Boston University, Boston, MA, USA
| | - K Hasuda
- Department of Physical Sciences, Aoyama Gakuin University, Tokyo, Japan
| | - F Hemrich
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany
| | - H Y Hsiao
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - S Ibryamov
- Department of Physics and Astronomy, Faculty of Natural Sciences, University of Shumen, Shumen, Bulgaria
| | - T R Irsmambetova
- Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Moscow, Russia
| | - D V Ivanov
- Institute of Applied Astronomy, Russian Academy of Sciences, St. Petersburg, Russia
| | - M D Joner
- Department of Physics and Astronomy, Brigham Young University, Provo, UT, USA
| | - G N Kimeridze
- Abastumani Observatory, Mt. Kanobili, Abastumani, Georgia
| | | | - J Knött
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany
| | - E N Kopatskaya
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - S O Kurtanidze
- Abastumani Observatory, Mt. Kanobili, Abastumani, Georgia.,Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Heidelberg, Germany
| | - A Kurtenkov
- Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria
| | - T Kuutma
- Centro de Estudios de Física del Cosmos de Aragón, Teruel, Spain
| | - E G Larionova
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - S Leonini
- Montarrenti Observatory, Siena, Italy
| | - H C Lin
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - C Lorey
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany
| | - K Mannheim
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany.,Lehrstuhl für Astronomie, Universität Würzburg, Würzburg, Germany
| | - G Marino
- Gruppo Astrofili Catanesi (GAC), Catania, Italy.,Wild Boar Remote Observatory, Florence, Italy
| | - M Minev
- Department of Astronomy, Faculty of Physics, University of Sofia, Sofia, Bulgaria
| | | | - D A Morozova
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - A A Nikiforova
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.,Pulkovo Observatory, St. Petersburg, Russia
| | - M G Nikolashvili
- Abastumani Observatory, Mt. Kanobili, Abastumani, Georgia.,Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Heidelberg, Germany
| | - E Ovcharov
- Department of Astronomy, Faculty of Physics, University of Sofia, Sofia, Bulgaria
| | - R Papini
- Wild Boar Remote Observatory, Florence, Italy
| | - T Pursimo
- Nordic Optical Telescope, Santa Cruz de Tenerife, Spain.,Department of Physics and Astronomy, Aarhus University, Aarhus C, Denmark
| | - I Rahimov
- Institute of Applied Astronomy, Russian Academy of Sciences, St. Petersburg, Russia
| | - D Reinhart
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany
| | - T Sakamoto
- Department of Physical Sciences, Aoyama Gakuin University, Tokyo, Japan
| | - F Salvaggio
- Gruppo Astrofili Catanesi (GAC), Catania, Italy.,Wild Boar Remote Observatory, Florence, Italy
| | - E Semkov
- Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria
| | | | - L A Sigua
- Abastumani Observatory, Mt. Kanobili, Abastumani, Georgia
| | - R Steineke
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany
| | - M Stojanovic
- Astronomical Observatory Belgrade, Belgrade, Serbia
| | - A Strigachev
- Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria
| | - Y V Troitskaya
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - I S Troitskiy
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - A Tsai
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - A Valcheva
- Department of Astronomy, Faculty of Physics, University of Sofia, Sofia, Bulgaria
| | - A A Vasilyev
- Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia
| | - O Vince
- Astronomical Observatory Belgrade, Belgrade, Serbia
| | - L Waller
- Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany
| | - E Zaharieva
- Department of Astronomy, Faculty of Physics, University of Sofia, Sofia, Bulgaria
| | - R Chatterjee
- Department of Physics, Presidency University, Kolkata, India
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159
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Krishnarao D, Fox AJ, D'Onghia E, Wakker BP, Cashman FH, Howk JC, Lucchini S, French DM, Lehner N. Observations of a Magellanic Corona. Nature 2022; 609:915-918. [PMID: 36171382 PMCID: PMC9519455 DOI: 10.1038/s41586-022-05090-5] [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] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/13/2022] [Accepted: 07/08/2022] [Indexed: 11/15/2022]
Abstract
The Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) are the closest massive satellite galaxies of the Milky Way. They are probably on their first passage on an infalling orbit towards our Galaxy1 and trace the continuing dynamics of the Local Group2. Recent measurements of a high mass for the LMC (Mhalo ≈ 1011.1–11.4 M⊙)3–6 imply that the LMC should host a Magellanic Corona: a collisionally ionized, warm-hot gaseous halo at the virial temperature (105.3–5.5 K) initially extending out to the virial radius (100–130 kiloparsecs (kpc)). Such a corona would have shaped the formation of the Magellanic Stream7, a tidal gas structure extending over 200° across the sky2,8,9 that is bringing in metal-poor gas to the Milky Way10. Here we show evidence for this Magellanic Corona with a potential direct detection in highly ionized oxygen (O+5) and indirectly by means of triply ionized carbon and silicon, seen in ultraviolet (UV) absorption towards background quasars. We find that the Magellanic Corona is part of a pervasive multiphase Magellanic circumgalactic medium (CGM) seen in many ionization states with a declining projected radial profile out to at least 35 kpc from the LMC and a total ionized CGM mass of log10(MH II,CGM/M⊙) ≈ 9.1 ± 0.2. The evidence for the Magellanic Corona is a crucial step forward in characterizing the Magellanic group and its nested evolution with the Local Group. By analysing Hubble Space Telescope/Cosmic Origins Spectrograph spectra, evidence is provided for the presence of a Magellanic Corona surrounding the Large Magellanic Cloud, as predicted given its high mass.
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Affiliation(s)
- Dhanesh Krishnarao
- Space Telescope Science Institute, Baltimore, MD, USA. .,William H. Miller III Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA. .,Department of Physics, Colorado College, Colorado Springs, CO, USA.
| | - Andrew J Fox
- AURA for ESA, Space Telescope Science Institute, Baltimore, MD, USA
| | - Elena D'Onghia
- Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA
| | - Bart P Wakker
- Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA
| | | | - J Christopher Howk
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, IN, USA
| | - Scott Lucchini
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | | | - Nicolas Lehner
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, IN, USA
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160
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Melli A, Melosso M, Bizzocchi L, Alessandrini S, Jiang N, Tonolo F, Boi S, Castellan G, Sapienza C, Guillemin JC, Dore L, Puzzarini C. Rotational Spectra of Unsaturated Carbon Chains Produced by Pyrolysis: The Case of Propadienone, Cyanovinylacetylene, and Allenylacetylene. J Phys Chem A 2022; 126:6210-6220. [PMID: 36044202 PMCID: PMC9483987 DOI: 10.1021/acs.jpca.2c05018] [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] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
![]()
Several interstellar molecules are highly reactive unsaturated
carbon chains, which are unstable under terrestrial conditions. Laboratory
studies in support of their detection in space thus face the issue
of how to produce these species and how to correctly model their rotational
energy levels. In this work, we introduce a general approach for producing
and investigating unsaturated carbon chains by means of selected test
cases. We report a comprehensive theoretical/experimental spectroscopic
characterization of three species, namely, propadienone, cyanovinylacetylene,
and allenylacetylene, all of them being produced by means of flash
vacuum pyrolysis of a suitable precursor. For each species, quantum-chemical
calculations have been carried out with the aim of obtaining accurate
predictions of the missing spectroscopic information required to guide
spectral analysis and assignment. Rotational spectra of the title
molecules have been investigated up to 400 GHz by using a frequency-modulation
millimeter-/submillimeter-wave spectrometer, thus significantly extending
spectral predictions over a wide range of frequency and quantum numbers.
A comparison between our results and those available in the literature
points out the clear need of the reported laboratory measurements
at higher frequencies for setting up accurate line catalogs for astronomical
searches.
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Affiliation(s)
- Alessio Melli
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy.,Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy
| | - Mattia Melosso
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy.,Scuola Superiore Meridionale, Largo San Marcellino 10, 80138 Naples, Italy
| | - Luca Bizzocchi
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
| | - Silvia Alessandrini
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy.,Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy
| | - Ningjing Jiang
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
| | - Francesca Tonolo
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy.,Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy
| | - Salvatore Boi
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
| | - Giorgia Castellan
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
| | - Carlotta Sapienza
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
| | - Jean-Claude Guillemin
- Univ Rennes, Ecole Nationale Supérieure de Chimie de Rennes, CNRS, ISCR-UMR6226, F-35000 Rennes, France
| | - Luca Dore
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
| | - Cristina Puzzarini
- Dipartimento di Chimica "Giacomo Ciamician", Università di Bologna, Via F. Selmi 2, 40126 Bologna, Italy
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161
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Kohri K, Sekiguchi T, Wang S. Cosmological 21-cm line observations to test scenarios of super-Eddington accretion on to black holes being seeds of high-redshifted supermassive black holes. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043539] [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: 11/07/2022]
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162
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Okounkova M, Farr WM, Isi M, Stein LC. Constraining gravitational wave amplitude birefringence and Chern-Simons gravity with GWTC-2. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.044067] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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163
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Abstract
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The relative abundances of singly deuterated methanol
isotopologues,
[CH2DOH]/[CH3OD], in star-forming regions deviate
from the statistically expected ratio of 3. In Orion KL, the nearest
high-mass star-forming region to Earth, the singly deuterated methanol
ratio is about 1, and the cause for this observation has been explored
through theory for nearly three decades. We present high-angular resolution
observations of Orion KL using the Atacama Large Millimeter/submillimeter
Array to map small-scale changes in CH3OD column density
across the nebula, which provide a new avenue to examine the deuterium
chemistry during star and planet formation. By considering how CH3OD column densities vary with temperature, we find evidence
of chemical processes that can significantly alter the observed gas-phase
column densities. The astronomical data are compared with existing
theoretical work and support D–H exchange between CH3OH and heavy water (i.e., HDO and D2O) at methanol’s
hydroxyl site in the icy mantles of dust grains. The enhanced CH3OD column densities are localized to the Hot Core-SW region,
a pattern that may be linked to the coupled evolution of ice mantle
chemistry and star formation in giant molecular clouds. This work
provides new perspectives on deuterated methanol chemistry in Orion
KL and informs considerations that may guide future theoretical, experimental,
and observational work.
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Affiliation(s)
- Olivia H Wilkins
- Division of Chemistry and Chemical Engineering, California Institute of Technology, Pasadena, California 91125, United States
| | - Geoffrey A Blake
- Division of Chemistry and Chemical Engineering, California Institute of Technology, Pasadena, California 91125, United States.,Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, United States
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164
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He C, Luo Y, Doddipatla S, Yang Z, Millar TJ, Sun R, Kaiser RI. Gas-phase formation of silicon monoxide via non-adiabatic reaction dynamics and its role as a building block of interstellar silicates. Phys Chem Chem Phys 2022; 24:19761-19772. [PMID: 35971984 DOI: 10.1039/d2cp02188a] [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: 11/21/2022]
Abstract
Silicon monoxide (SiO) is classified as a key precursor and fundamental molecular building block to interstellar silicate nanoparticles, which play an essential role in the synthesis of molecular building blocks connected to the Origins of Life. In the cold interstellar medium, silicon monoxide is of critical importance in initiating a series of elementary chemical reactions leading to larger silicon oxides and eventually to silicates. To date, the fundamental formation mechanisms and chemical dynamics leading to gas phase silicon monoxide have remained largely elusive. Here, through a concerted effort between crossed molecular beam experiments and electronic structure calculations, it is revealed that instead of forming highly-stable silicon dioxide (SiO2), silicon monoxide can be formed via a barrierless, exoergic, single-collision event between ground state molecular oxygen and atomic silicon involving non-adiabatic reaction dynamics through various intersystem crossings. Our research affords persuasive evidence for a likely source of highly rovibrationally excited silicon monoxide in cold molecular clouds thus initiating the complex chain of exoergic reactions leading ultimately to a population of silicates at low temperatures in our Galaxy.
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Affiliation(s)
- Chao He
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Yuheng Luo
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Srinivas Doddipatla
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Zhenghai Yang
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Tom J Millar
- School of Mathematics and Physics, Queen's University Belfast, University Road, Belfast, BT7 1NN, UK
| | - Rui Sun
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
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165
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Paul D, Yang Z, Goettl SJ, Thomas AM, He C, Suits AG, Parker DH, Kaiser RI. Photodissociation Dynamics of Astrophysically Relevant Propyl Derivatives (C 3H 7X; X = CN, OH, HCO) at 157 nm Exploiting an Ultracompact Velocity Map Imaging Spectrometer: The (Iso)Propyl Channel. J Phys Chem A 2022; 126:5768-5775. [PMID: 35993843 DOI: 10.1021/acs.jpca.2c04430] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
The photodissociation dynamics of astrophysically relevant propyl derivatives (C3H7X; X = CN, OH, HCO) at 157 nm exploiting an ultracompact velocity map imaging (UVMIS) setup has been reported. The successful operation of UVMIS allowed the exploration of the 157 nm photodissociation of six (iso)propyl systems─n/i-propyl cyanide (C3H7CN), n/i-propyl alcohol (C3H7OH), and (iso)butanal (C3H7CHO)─to explore the C3H7 loss channel. The distinct center-of-mass translational energy distributions for the i-C3H7X (X= CN, OH, HCO) could be explained through preferential excitation of the low frequency C-H bending modes of the formyl moiety compared to the higher frequency stretching of the cyano and hydroxy moieties. Although the ionization energy of the n-C3H7 radical exceeds the energy of a 157 nm photon, C3H7+ was observed in the n-C3H7X (X = CN, OH, HCO) systems as a result of photoionization of vibrationally "hot" n-C3H7 fragments, photoionization of i-C3H7 after a hydrogen shift in vibrationally "hot" n-C3H7 radicals, and/or two-photon ionization. Our experiments reveal that at least the isopropyl radical (i-C3H7) and possibly the normal propyl radical (n-C3H7) should be present in the interstellar medium and hence searched for by radio telescopes.
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Affiliation(s)
- Dababrata Paul
- Department of Chemistry, University of Hawai'i at Manoa, Honolulu, Hawaii 96822, United States
| | - Zhenghai Yang
- Department of Chemistry, University of Hawai'i at Manoa, Honolulu, Hawaii 96822, United States
| | - Shane J Goettl
- Department of Chemistry, University of Hawai'i at Manoa, Honolulu, Hawaii 96822, United States
| | - Aaron M Thomas
- Department of Chemistry, University of Hawai'i at Manoa, Honolulu, Hawaii 96822, United States
| | - Chao He
- Department of Chemistry, University of Hawai'i at Manoa, Honolulu, Hawaii 96822, United States
| | - Arthur G Suits
- Department of Chemistry, University of Missouri, Columbia, Missouri 65211, United States
| | - David H Parker
- Department of Laser Physics, Institute for Molecules and Materials, Radboud University, Nijmegen 6500, The Netherlands
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawai'i at Manoa, Honolulu, Hawaii 96822, United States
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166
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Todd ZR. Sources of Nitrogen-, Sulfur-, and Phosphorus-Containing Feedstocks for Prebiotic Chemistry in the Planetary Environment. Life (Basel) 2022; 12:1268. [PMID: 36013447 DOI: 10.3390/life12081268] [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] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/30/2022] [Revised: 08/13/2022] [Accepted: 08/17/2022] [Indexed: 11/21/2022]
Abstract
Biochemistry on Earth makes use of the key elements carbon, hydrogen, oxygen, nitrogen, phosphorus, and sulfur (or CHONPS). Chemically accessible molecules containing these key elements would presumably have been necessary for prebiotic chemistry and the origins of life on Earth. For example, feedstock molecules including fixed nitrogen (e.g., ammonia, nitrite, nitrate), accessible forms of phosphorus (e.g., phosphate, phosphite, etc.), and sources of sulfur (e.g., sulfide, sulfite) may have been necessary for the origins of life, given the biochemistry seen in Earth life today. This review describes potential sources of nitrogen-, sulfur-, and phosphorus-containing molecules in the context of planetary environments. For the early Earth, such considerations may be able to aid in the understanding of our own origins. Additionally, as we learn more about potential environments on other planets (for example, with upcoming next-generation telescope observations or new missions to explore other bodies in our Solar System), evaluating potential sources for elements necessary for life (as we know it) can help constrain the potential habitability of these worlds.
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167
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Dagdigian PJ. Theoretical Investigation of Rotationally Inelastic Collisions of OH( X2Π) with Hydrogen Atoms. J Chem Phys 2022; 157:104305. [DOI: 10.1063/5.0110724] [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: 11/14/2022] Open
Abstract
State-to-state cross sections and rate coefficients for transitions between rotational/fine- structure levels of OH(X2Π) induced by collisions with atomic hydrogen are reported in this work. The scattering calculations take into account the full open-shell character of the OH + H system and include the four potential energy surfaces (1A′, 1A′′, 3A′, 3A′′) that correlate with the OH(X2Π) + H(2S) asymptote. Three of these surfaces are repulsive, while the deep H2O well is present on one surface (1A′). The OH + H potential energy curves calculated by Alexander et al. [J. Chem. Phys. 121, 5221 (2004)] are employed in this work. Time independent quantum scattering calculations were performed using the quantum statistical method of Manolopoulos and co-workers [Chem. Phys. Lett. 343, 356 (2001)] because of the presence of the deep H2O well. The computed cross sections include contributions from direct scattering, as well formation and decay of a transient collision complex since the transient HO-H complex is expected to decay nonreactively. Rate coefficients for OH-H inelastic collisions are of interest for astrophysical applications.
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Affiliation(s)
- Paul J. Dagdigian
- Department of Chemistry, Johns Hopkins University, United States of America
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168
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Joeris K, Schönau L, Keulen M, Born P, Kollmer JE. The influence of interparticle cohesion on rebounding slow impacts on rubble pile asteroids. NPJ Microgravity 2022; 8:36. [PMID: 35978020 PMCID: PMC9385662 DOI: 10.1038/s41526-022-00221-8] [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] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/20/2021] [Accepted: 07/13/2022] [Indexed: 11/18/2022] Open
Abstract
The ballistic sorting effect has been proposed to be a driver behind the observed size sorting on the rubble pile asteroid Itokawa. This effect depends on the inelasticity of slow collisions with granular materials. The inelasticity of a collision with a granular material, in turn, depends on grain size. Here we argue that determining the inelasticity of such collisions in an asteroid-like environment is a nontrivial task. We show non-monotonic dependency of the coefficient of restitution (COR) on target particle size using experiments in microgravity. Employing numerical simulations, we explain these results with the growing influence of adhesion for smaller-sized particles. We conclude that there exists an optimum impactor to target particle size ratio for ballistic sorting.
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Affiliation(s)
- Kolja Joeris
- Experimentelle Astrophysik, Universität Duisburg-Essen, Lotharstr. 1-21, 47057, Duisburg, Germany.
| | - Laurent Schönau
- Experimentelle Astrophysik, Universität Duisburg-Essen, Lotharstr. 1-21, 47057, Duisburg, Germany
| | - Matthias Keulen
- Experimentelle Astrophysik, Universität Duisburg-Essen, Lotharstr. 1-21, 47057, Duisburg, Germany
| | - Philip Born
- Institut für Materialphysik im Weltraum, Deutsches Zentrum für Luft- und Raumfahrt (DLR), 51170, Köln, Germany
| | - Jonathan E Kollmer
- Experimentelle Astrophysik, Universität Duisburg-Essen, Lotharstr. 1-21, 47057, Duisburg, Germany
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169
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Tian S. Cosmological consequences of a scalar field with oscillating equation of state. IV. Primordial nucleosynthesis and the deuterium problem. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043524] [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: 11/07/2022]
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170
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Nietiadi ML, Rosandi Y, Bringa EM, Urbassek HM. Collisions between CO, CO[Formula: see text], H[Formula: see text]O and Ar ice nanoparticles compared by molecular dynamics simulation. Sci Rep 2022; 12:13858. [PMID: 35974128 PMCID: PMC9381553 DOI: 10.1038/s41598-022-18039-5] [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] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/06/2022] [Accepted: 08/04/2022] [Indexed: 12/01/2022] Open
Abstract
Molecular dynamics simulations are used to study collisions between amorphous ice nanoparticles consisting of CO, CO[Formula: see text], Ar and H[Formula: see text]O. The collisions are always sticking for the nanoparticle size (radius of 20 nm) considered. At higher collision velocities, the merged clusters show strong plastic deformation and material mixing in the collision zone. Collision-induced heating influences the collision outcome. Partial melting of the merged cluster in the collision zone contributes to energy dissipation and deformation. Considerable differences exist-even at comparable collision conditions-between the ices studied here. The number of ejecta emitted during the collision follows the trend in triple-point temperatures and increases exponentially with the NP temperature.
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Affiliation(s)
- Maureen L. Nietiadi
- Physics Department and Research Center OPTIMAS, University Kaiserslautern, Erwin-Schrödinger-Straße, 67663 Kaiserslautern, Germany
| | - Yudi Rosandi
- Department of Geophysics, Universitas Padjadjaran, Jatinangor, Sumedang 45363 Indonesia
| | - Eduardo M. Bringa
- CONICET and Facultad de Ingenería, Universidad de Mendoza, 5500 Mendoza, Argentina
- Centro de Nanotecnología Aplicada, Facultad de Ciencias, Universidad Mayor, 8580745 Santiago, Chile
| | - Herbert M. Urbassek
- Physics Department and Research Center OPTIMAS, University Kaiserslautern, Erwin-Schrödinger-Straße, 67663 Kaiserslautern, Germany
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171
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Kader Z, Leung C, Dobbs M, Masui KW, Michilli D, Mena-Parra J, Mckinven R, Ng C, Bandura K, Bhardwaj M, Brar C, Cassanelli T, Chawla P, Dong FA, Good D, Kaspi V, Lanman AE, Lin HH, Meyers BW, Pearlman AB, Pen UL, Petroff E, Pleunis Z, Rafiei-Ravandi M, Rahman M, Sanghavi P, Scholz P, Shin K, Siegel S, Smith KM, Stairs I, Tendulkar SP, Vanderlinde K, Wulf D. High-time resolution search for compact objects using fast radio burst gravitational lens interferometry with CHIME/FRB. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043016] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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172
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Leung C, Kader Z, Masui KW, Dobbs M, Michilli D, Mena-Parra J, Mckinven R, Ng C, Bandura K, Bhardwaj M, Brar C, Cassanelli T, Chawla P, Dong FA, Good D, Kaspi V, Lanman AE, Lin HH, Meyers BW, Pearlman AB, Pen UL, Petroff E, Pleunis Z, Rafiei-Ravandi M, Rahman M, Sanghavi P, Scholz P, Shin K, Siegel S, Smith KM, Stairs I, Tendulkar SP, Vanderlinde K. Constraining primordial black holes using fast radio burst gravitational-lens interferometry with CHIME/FRB. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043017] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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173
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Trani AA, Rieder S, Tanikawa A, Iorio G, Martini R, Karelin G, Glanz H, Portegies Zwart S. Revisiting the common envelope evolution in binary stars: A new semianalytic model for
N
-body and population synthesis codes. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043014] [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: 11/07/2022]
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174
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Affiliation(s)
| | - Els Peeters
- grid.39381.300000 0004 1936 8884Department of Physics & Astronomy, University of Western Ontario, London, ON N6A 3K7 Canada ,grid.39381.300000 0004 1936 8884Institute for Earth and Space Exploration, University of Western Ontario, London, ON N6A 3K7 Canada ,grid.422128.f0000 0001 2115 2810SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043 USA
| | - Jan Cami
- grid.39381.300000 0004 1936 8884Department of Physics & Astronomy, University of Western Ontario, London, ON N6A 3K7 Canada ,grid.39381.300000 0004 1936 8884Institute for Earth and Space Exploration, University of Western Ontario, London, ON N6A 3K7 Canada ,grid.422128.f0000 0001 2115 2810SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043 USA
| | - Timothy W. Schmidt
- grid.1005.40000 0004 4902 0432School of Chemistry, UNSW, Sydney, NSW 2052 Australia
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175
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Wang Y, Gilson EP, Ebrahimi F, Goodman J, Caspary KJ, Winarto HW, Ji H. Identification of a non-axisymmetric mode in laboratory experiments searching for standard magnetorotational instability. Nat Commun 2022; 13:4679. [PMID: 35945242 DOI: 10.1038/s41467-022-32278-0] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/04/2022] [Accepted: 07/25/2022] [Indexed: 11/13/2022] Open
Abstract
The standard magnetorotational instability (SMRI) is a promising mechanism for turbulence and rapid accretion in astrophysical disks. It is a magnetohydrodynamic (MHD) instability that destabilizes otherwise hydrodynamically stable disk flow. Due to its microscopic nature at astronomical distances and stringent requirements in laboratory experiments, SMRI has remained unconfirmed since its proposal, despite its astrophysical importance. Here we report a nonaxisymmetric MHD instability in a modified Taylor-Couette experiment. To search for SMRI, a uniform magnetic field is imposed along the rotation axis of a swirling liquid-metal flow. The instability initially grows exponentially, becoming prominent only for sufficient flow shear and moderate magnetic field. These conditions for instability are qualitatively consistent with SMRI, but at magnetic Reynolds numbers below the predictions of linear analyses with periodic axial boundaries. Three-dimensional numerical simulations, however, reproduce the observed instability, indicating that it grows linearly from the primary axisymmetric flow modified by the applied magnetic field. Magnetohydrodynamic instabilities are related to different characteristics and behavior of fluids. Here the authors report an experiment and simulation combined study of a global non-axisymmetric MHD instability that exists at sufficiently large rotation rates and intermediate magnetic field strengths.
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176
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Du P, Egaña-Ugrinovic D, Essig R, Fragione G, Perna R. Searching for ultra-light bosons and constraining black hole spin distributions with stellar tidal disruption events. Nat Commun 2022; 13:4626. [PMID: 35941178 DOI: 10.1038/s41467-022-32301-4] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/18/2022] [Accepted: 07/22/2022] [Indexed: 11/30/2022] Open
Abstract
Stars that pass close to the supermassive black holes located in the center of galaxies can be disrupted by tidal forces, leading to flares that are observed as bright transient events in sky surveys. The rate for these events to occur depends on the black hole spins, which in turn can be affected by ultra-light bosons due to superradiance. We perform a detailed analysis of these effects and show that searches for stellar tidal disruptions have the potential to uncover the existence of ultra-light bosons. In particular, we find that upcoming stellar tidal disruption rate measurements by the Vera Rubin Observatory’s Legacy Survey of Space and Time can be used to either discover or rule out bosons with masses ranging from 10−20 to 10−18 eV. Our analysis also indicates that these measurements may be used to constrain a variety of supermassive black hole spin distributions and determine if close-to maximal spins are preferred. Stellar tidal disruption events (TDEs) occur when stars pass close enough to supermassive black holes. Here, the authors show that future searches TDEs have potential to uncover the existence of ultralight bosons.
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177
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Lourenço O, Lenzi C, Frederico T, Dutra M. Dark matter effects on tidal deformabilities and moment of inertia in a hadronic model with short-range correlations. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043010] [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: 11/07/2022]
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178
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Zhang Y, Michel P, Barnouin OS, Roberts JH, Daly MG, Ballouz RL, Walsh KJ, Richardson DC, Hartzell CM, Lauretta DS. Inferring interiors and structural history of top-shaped asteroids from external properties of asteroid (101955) Bennu. Nat Commun 2022; 13:4589. [PMID: 35933392 PMCID: PMC9357032 DOI: 10.1038/s41467-022-32288-y] [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] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/12/2021] [Accepted: 07/20/2022] [Indexed: 11/30/2022] Open
Abstract
Asteroid interiors play a key role in our understanding of asteroid formation and evolution. As no direct interior probing has been done yet, characterisation of asteroids’ interiors relies on interpretations of external properties. Here we show, by numerical simulations, that the top-shaped rubble-pile asteroid (101955) Bennu’s geophysical response to spinup is highly sensitive to its material strength. This allows us to infer Bennu’s interior properties and provide general implications for top-shaped rubble piles’ structural evolution. We find that low-cohesion (≲0.78 Pa at surface and ≲1.3 Pa inside) and low-friction (friction angle ≲ 35∘) structures with several high-cohesion internal zones can consistently account for all the known geophysical characteristics of Bennu and explain the absence of moons. Furthermore, we reveal the underlying mechanisms that lead to different failure behaviours and identify the reconfiguration pathways of top-shaped asteroids as functions of their structural properties that either facilitate or prevent the formation of moons. Asteroid interiors are key to understand their formation and evolution. Here, the authors show that numerically simulated low-cohesion and low-friction structures with several high-cohesion internal zones can explain asteroid Bennu’s geophysical characteristics and the absence of the moons.
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Affiliation(s)
- Yun Zhang
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France. .,Department of Aerospace Engineering, University of Maryland, College Park, MD, USA.
| | - Patrick Michel
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France
| | - Olivier S Barnouin
- The Johns Hopkins University, Applied Physics Laboratory, Laurel, MD, USA
| | - James H Roberts
- The Johns Hopkins University, Applied Physics Laboratory, Laurel, MD, USA
| | - Michael G Daly
- The Centre for Research in Earth and Space Science, York University, Toronto, ON, Canada
| | - Ronald-L Ballouz
- The Johns Hopkins University, Applied Physics Laboratory, Laurel, MD, USA.,Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | | | - Christine M Hartzell
- Department of Aerospace Engineering, University of Maryland, College Park, MD, USA
| | - Dante S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
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179
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Ginolfi M, Piconcelli E, Zappacosta L, Jones GC, Pentericci L, Maiolino R, Travascio A, Menci N, Carniani S, Rizzo F, Arrigoni Battaia F, Cantalupo S, De Breuck C, Graziani L, Knudsen K, Laursen P, Mainieri V, Schneider R, Stanley F, Valiante R, Verhamme A. Detection of companion galaxies around hot dust-obscured hyper-luminous galaxy W0410-0913. Nat Commun 2022; 13:4574. [PMID: 35931777 PMCID: PMC9355969 DOI: 10.1038/s41467-022-32297-x] [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] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/12/2022] [Accepted: 07/22/2022] [Indexed: 11/28/2022] Open
Abstract
The phase transition between galaxies and quasars is often identified with the rare population of hyper-luminous, hot dust-obscured galaxies. Galaxy formation models predict these systems to grow via mergers, that can deliver large amounts of gas toward their centers, induce intense bursts of star formation and feed their supermassive black holes. Here we report the detection of 24 galaxies emitting Lyman-α emission on projected physical scales of about 400 kpc around the hyper-luminous hot dust-obscured galaxy W0410-0913, at redshift z = 3.631, using Very Large Telescope observations. While this indicates that W0410-0913 evolves in a very dense environment, we do not find clear signs of mergers that could sustain its growth. Data suggest that if mergers occurred, as models expect, these would involve less massive satellites, with only a moderate impact on the internal interstellar medium of W0410-0913, which is sustained by a rotationally-supported fast-rotating molecular disk, as Atacama Large Millimeter Array observations suggest. Lyman-alpha emission is one of the observational probes for the high-redshift universe. Here, the authors show several Lyman-alpha emitting companion galaxies around the hot dust-obscured galaxy W0410-091 suggesting that the galaxy evolves in a very dense environment.
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Affiliation(s)
- M Ginolfi
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany.
| | - E Piconcelli
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - L Zappacosta
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - G C Jones
- Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 4RH, UK.,Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge, CB3 0HE, UK.,Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
| | - L Pentericci
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - R Maiolino
- Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge, CB3 0HE, UK.,Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
| | - A Travascio
- Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126, Milano, Italy
| | - N Menci
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - S Carniani
- Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126, Pisa, Italy
| | - F Rizzo
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark.,Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200, Copenhagen N, Denmark
| | - F Arrigoni Battaia
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, D-85748, Garching bei München, Germany
| | - S Cantalupo
- Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126, Milano, Italy
| | - C De Breuck
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany
| | - L Graziani
- Dipartimento di Fisica, Sapienza, Universita di Roma, Piazzale Aldo Moro 5, I-00185, Roma, Italy
| | - K Knudsen
- Department of Space, Earth, and Environment, Chalmers University of Technology, Onsala Space Observatory, SE-439 92, Onsala, Sweden
| | - P Laursen
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark.,Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200, Copenhagen N, Denmark
| | - V Mainieri
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany
| | - R Schneider
- Dipartimento di Fisica, Sapienza, Universita di Roma, Piazzale Aldo Moro 5, I-00185, Roma, Italy
| | - F Stanley
- Sorbonne Université, UPMC Université Paris 6 & CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98b boulevard Arago, 75014, Paris, France
| | - R Valiante
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - A Verhamme
- Observatoire de Genéve, Université de Genève, 51 Ch. des Maillettes, 1290, Versoix, Switzerland
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180
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Gustafsson B. Chemical Tracing and the Origin of Carbon in the Galactic Disk. Universe 2022; 8:409. [DOI: 10.3390/universe8080409] [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] [Subscribe] [Scholar Register] [Indexed: 02/05/2023]
Abstract
A basic problem in studies of the evolution of chemical elements in galaxies is the uncertainties in the yields of elements produced by different types of stars. The possibilities of tracing the sites producing chemical elements and corresponding yields in stellar populations by studying ratios of abundances in stars of different ages and metallicities, with an approach with minimal assumptions concerning the yields, is explored by means of simple models of Galactic chemical evolution. Elemental abundances of carbon and oxygen, obtained by recent observations of samples of solar-type stars with estimated ages in the thin disk of the Galaxy, are analysed. Constraints on the yields from winds of intermediate-mass stars and of hot massive stars, including core-collapse supernovae, are derived. It is found that a dominating contribution of carbon from massive stars is most probable, although stars in the mass interval of two to three solar masses may have provided some amounts of carbon in the Sun. The results are consistent with those obtained by using theoretical yields and more elaborate models of Galactic evolution. The uncertainties as regards the mixing of stellar populations due to migration of stars in the Galactic disk may be important for the conclusions. Variations in the star formation rates, lack of chemical homogeneity in the Galactic gas, the inflow of gas from the intergalactic space and possible variations in the Initial mass function may also limit conclusions about the sites and their yields. Very accurate abundance ratios and the determination of stellar ages provide further important constraints on the yields.
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181
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Lacinbala O, Féraud G, Vincent J, Pino T. Aromatic and Acetylenic C-H or C-D Stretching Bands Anharmonicity Detection of Phenylacetylene by UV Laser-Induced Vibrational Emission. J Phys Chem A 2022; 126:4891-4901. [PMID: 35880827 DOI: 10.1021/acs.jpca.2c01436] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
The anharmonic infrared (IR) emission spectra of phenylacetylene C6H5CCH and an isotopologue C6H5CCD induced by 193 nm UV excitation have been investigated in the gas phase. The study has been operated with a homemade IR spectrometer enabling to record time- and wavelength-resolved spectra between 2.5 and 4.5 μm, emitted all along the collisional cooling. The analysis is supported by a kinetic Monte Carlo simulation in the vibrational harmonic approximation. For both species, the anharmonic shifts of the acetylenic C-H or C-D stretching modes and the aromatic C-H stretching modes are studied for band positions and bandwidths in terms of the internal energy. For C6H5CCD, the internal energy dependence of the emission intensity band ratio is investigated and rationalized. This work demonstrates the potential of time-resolved IR emission spectroscopy to explore anharmonicity of astrophysically relevant molecules.
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Affiliation(s)
- Ozan Lacinbala
- Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - Géraldine Féraud
- CNRS, LERMA, Sorbonne Université, Observatoire de Paris, Université PSL, F-75005, Paris, France
| | - Julien Vincent
- Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - Thomas Pino
- Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay, CNRS, 91405 Orsay, France
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182
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Baltus G, Janquart J, Lopez M, Narola H, Cudell JR. Convolutional neural network for gravitational-wave early alert: Going down in frequency. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.042002] [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: 11/07/2022]
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183
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Acosta-tripailao B, Max-moerbeck W, Pastén D, Moya PS. Assigning Degrees of Stochasticity to Blazar Light Curves in the Radio Band Using Complex Networks. Entropy 2022; 24:1063. [PMID: 36010727 PMCID: PMC9407290 DOI: 10.3390/e24081063] [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] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/31/2022] [Revised: 04/27/2022] [Accepted: 05/01/2022] [Indexed: 11/16/2022]
Abstract
We focus on characterizing the high-energy emission mechanisms of blazars by analyzing the variability in the radio band of the light curves of more than a thousand sources. We are interested in assigning complexity parameters to these sources, modeling the time series of the light curves with the method of the Horizontal Visibility Graph (HVG), which allows us to obtain properties from degree distributions, such as a characteristic exponent to describe its stochasticity and the Kullback–Leibler Divergence (KLD), presenting a new perspective to the methods commonly used to study Active Galactic Nuclei (AGN). We contrast these parameters with the excess variance, which is an astronomical measurement of variability in light curves; at the same time, we use the spectral classification of the sources. While it is not possible to find significant correlations with the excess variance, the degree distributions extracted from the network are detecting differences related to the spectral classification of blazars. These differences suggest a chaotic behavior in the time series for the BL Lac sources and a correlated stochastic behavior in the time series for the FSRQ sources. Our results show that complex networks may be a valuable alternative tool to study AGNs according to the variability of their energy output.
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184
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Kahremany S, Hofmann L, Gruzman A, Dinkova-Kostova AT, Cohen G. NRF2 in dermatological disorders: Pharmacological activation for protection against cutaneous photodamage and photodermatosis. Free Radic Biol Med 2022; 188:262-276. [PMID: 35753587 PMCID: PMC9350913 DOI: 10.1016/j.freeradbiomed.2022.06.238] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Submit a Manuscript] [Subscribe] [Scholar Register] [Received: 04/26/2022] [Revised: 06/16/2022] [Accepted: 06/21/2022] [Indexed: 01/27/2023]
Abstract
The skin barrier and its endogenous protective mechanisms cope daily with exogenous stressors, of which ultraviolet radiation (UVR) poses an imminent danger. Although the skin is able to reduce the potential damage, there is a need for comprehensive strategies for protection. This is particularly important when developing pharmacological approaches to protect against photocarcinogenesis. Activation of NRF2 has the potential to provide comprehensive and long-lasting protection due to the upregulation of numerous cytoprotective downstream effector proteins that can counteract the damaging effects of UVR. This is also applicable to photodermatosis conditions that exacerbate the damage caused by UVR. This review describes the alterations caused by UVR in normal skin and photosensitive disorders, and provides evidence to support the development of NRF2 activators as pharmacological treatments. Key natural and synthetic activators with photoprotective properties are summarized. Lastly, the gap in knowledge in research associated with photodermatosis conditions is highlighted.
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Affiliation(s)
- Shirin Kahremany
- Department of Chemistry, Faculty of Exact Sciences, Bar-Ilan University, Ramat-Gan, 5290002, Israel; The Skin Research Institute, The Dead Sea and Arava Science Center, Masada, 86910, Israel
| | - Lukas Hofmann
- Department of Chemistry, Faculty of Exact Sciences, Bar-Ilan University, Ramat-Gan, 5290002, Israel
| | - Arie Gruzman
- Department of Chemistry, Faculty of Exact Sciences, Bar-Ilan University, Ramat-Gan, 5290002, Israel
| | - Albena T Dinkova-Kostova
- Jacqui Wood Cancer Centre, Division of Cellular Medicine, School of Medicine, University of Dundee, Dundee, UK; Department of Pharmacology and Molecular Sciences and Department of Medicine, Johns Hopkins University School of Medicine, Baltimore, USA
| | - Guy Cohen
- The Skin Research Institute, The Dead Sea and Arava Science Center, Masada, 86910, Israel; Ben-Gurion University of the Negev, Eilat Campus, Eilat, 8855630, Israel.
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185
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Benisty D. Testing modified gravity via Yukawa potential in two body problem: Analytical solution and observational constraints. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043001] [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: 11/07/2022]
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186
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Zhu C, Peng C, Wu W. Lagrangian meshfree particle method (SPH) based simulation for granular flow in a rotating drum with regularized μ(I) elastoplastic model. POWDER TECHNOL 2022. [DOI: 10.1016/j.powtec.2022.117699] [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: 11/26/2022]
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187
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Chen X. Why do we study black holes? Chin Sci Bull 2022. [DOI: 10.1360/tb-2022-0792] [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: 11/09/2022]
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188
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Kubo A, Nishizawa J, Ikeda-Fukazawa T. Effects of interstitial water on phase transition of forsterite glass. Chem Phys Lett 2022. [DOI: 10.1016/j.cplett.2022.139932] [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: 11/25/2022]
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189
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Yuu S, Umekage T. Onset mechanism of granular avalanches in inclining layers using a continuum model. ADV POWDER TECHNOL 2022. [DOI: 10.1016/j.apt.2022.103659] [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: 11/28/2022]
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190
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191
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Shamir L. Asymmetry in Galaxy Spin Directions—Analysis of Data from DES and Comparison to Four Other Sky Surveys. Universe 2022; 8:397. [DOI: 10.3390/universe8080397] [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] [Subscribe] [Scholar Register] [Indexed: 02/01/2023]
Abstract
The paper shows an analysis of the large-scale distribution of galaxy spin directions of 739,286 galaxies imaged by DES. The distribution of the spin directions of the galaxies exhibits a large-scale dipole axis. Comparison of the location of the dipole axis to a similar analysis with data from SDSS, Pan-STARRS, and DESI Legacy Survey shows that all sky surveys exhibit dipole axes within 52° or less from each other, well within 1σ error, while non-random distribution is unexpected, the findings are consistent across all sky surveys, regardless of the telescope or whether the data were annotated manually or automatically. Possible errors that can lead to the observation are discussed. The paper also discusses previous studies showing opposite conclusions and analyzes the decisions that led to these results. Although the observation is provocative, and further research will be required, the existing evidence justifies considering the contention that galaxy spin directions as observed from Earth are not necessarily randomly distributed. Possible explanations can be related to mature cosmological theories, but also to the internal structure of galaxies.
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192
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Ershkov S, Leshchenko D, Rachinskaya A. Capture in Regime of a Trapped Motion with Further Inelastic Collision for Finite-Sized Asteroid in ER3BP. Symmetry (Basel) 2022; 14:1548. [DOI: 10.3390/sym14081548] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/17/2022] Open
Abstract
The application of a modern solving algorithm or method of resolving dynamical equations for small projectile of finite sizes orbiting to be captured in a trapped zigzaging oscillations on orbit around the another large asteroid and in a further inelastic colliding scenario with him (using a formulation of the elliptic restricted three-body problem, ER3BP) is studied semi-analytically. Herein, two primaries MSun and mp (mp < MSun) revolve around their barycenter on Keplerian orbits with low eccentricities. A smaller body (projectile for attacking a large asteroid) is supposed to be a solid, almost symmetric ellipsoid, having the gravitational potential of the MacCullagh type. Our aim is to develop a previously introduced solving procedure and to investigate the updated dynamics of the projectile captured to a trapped dynamical resonance, thereby having the inelastic collision of a small projectile orbiting on quasi-stable elliptic orbits around the large asteroid, mp.
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193
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Sabyr A, Hill JC, Bolliet B. Inverse-Compton scattering of the cosmic infrared background. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.023529] [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: 11/07/2022]
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194
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Berteaud J, Calore F, Iguaz J, Serpico P, Siegert T. Strong constraints on primordial black hole dark matter from 16 years of INTEGRAL/SPI observations. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.023030] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/06/2022]
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195
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Coimbra-araújo CH, dos Anjos RC. Ultra-High-Energy Particles at the Border of Kerr Black Holes Triggered by Magnetocentrifugal Winds. Galaxies 2022; 10:84. [DOI: 10.3390/galaxies10040084] [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] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
Abstract
The source, origin, and acceleration mechanisms of ultra-high-energy cosmic rays (UHECR) (E>1020 eV, beyond the GZK limit) remain uncertain and unclear. The main explanations are associated with particular mechanisms, such as the Fermi mechanism, in which charged particles could be accelerated by clouds of magnetized gas moving within our Galaxy, or by the magnetic reconnection of field lines at, e.g., the core of high-energy astrophysical sources, where the topology of the magnetic field is rearranged and magnetic energy is converted into kinetic energy. However, the recent observation of extragalactic neutrinos may suggest that the source of UHECRs is likely an extragalactic supermassive black hole. In the present work, we propose that charged particles can be accelerated to ultrahigh energies in marginally bound orbits near extreme rotating black holes and could be triggered by collisions of magnetocentrifugal winds; the accretion disk surrounding the black hole would provide such winds. The ultra-high-energy process is governed by the frame-dragging effects of the black hole spacetime.
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196
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Biswas S, Gabrielli E, Mele B. Dark Photon Searches via Higgs Boson Production at the LHC and Beyond. Symmetry (Basel) 2022; 14:1522. [DOI: 10.3390/sym14081522] [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: 12/10/2022] Open
Abstract
Many scenarios beyond the standard model, aiming to solve long-standing cosmological and particle physics problems, suggest that dark matter might experience long-distance interactions mediated by an unbroken dark U(1) gauge symmetry, hence foreseeing the existence of a massless dark photon. Contrary to the massive dark photon, a massless dark photon can only couple to the standard model sector by means of effective higher dimensional operators. Massless dark photon production at colliders will then in general be suppressed at low energy by a UV energy scale, which is of the order of the masses of portal (messenger) fields connecting the dark and the observable sectors. A violation of this expectation is provided by dark photon production mediated by the Higgs boson, thanks to the non-decoupling Higgs properties. Higgs boson production at colliders, followed by the Higgs decay into a photon and a dark photon, provides then a very promising production mechanism for the dark photon discovery, being insensitive in particular regimes to the UV scale of the new physics. This decay channel gives rise to a peculiar signature characterized by a monochromatic photon with energy half the Higgs mass (in the Higgs rest frame) plus missing energy. We show how such resonant photon-plus-missing-energy signature can uniquely be connected to a dark photon production. Higgs boson production and decay into a photon and a dark photon as a source of dark photons is reviewed at the Large Hadron Collider, in light of the present bounds on the corresponding signature by the CMS and ATLAS collaborations. Perspectives for the dark photon production in Higgs-mediated processes at future e+e− colliders are also discussed.
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197
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Li S, Ozkan-Aydin Y, Xiao C, Small G, Gynai HN, Li G, Rieser JM, Laguna P, Goldman DI. Field-mediated locomotor dynamics on highly deformable surfaces. Proc Natl Acad Sci U S A 2022; 119:e2113912119. [PMID: 35857871 DOI: 10.1073/pnas.2113912119] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/22/2023] Open
Abstract
Studies of active matter-systems consisting of individuals or ensembles of internally driven and damped locomotors-are of interest to physicists studying nonequilibrium dynamics, biologists interested in individuals and swarm locomotion, and engineers designing robot controllers. While principles governing active systems on hard ground or within fluids are well studied, another class of systems exists at deformable interfaces. Such environments can display mixes of fluid-like and elastic features, leading to locomotor dynamics that are strongly influenced by the geometry of the surface, which, in itself, can be a dynamical entity. To gain insight into principles by which locomotors are influenced via a deformation field alone (and can influence other locomotors), we study robot locomotion on an elastic membrane, which we propose as a model of active systems on highly deformable interfaces. As our active agent, we use a differential driven wheeled robotic vehicle which drives straight on flat homogeneous surfaces, but reorients in response to environmental curvature. We monitor the curvature field-mediated dynamics of a single vehicle interacting with a fixed deformation as well as multiple vehicles interacting with each other via local deformations. Single vehicles display precessing orbits in centrally deformed environments, while multiple vehicles influence each other by local deformation fields. The active nature of the system facilitates a differential geometry-inspired mathematical mapping from the vehicle dynamics to those of test particles in a fictitious "spacetime," allowing further understanding of the dynamics and how to control agent interactions to facilitate or avoid multivehicle membrane-induced cohesion.
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198
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García-Sánchez M, Jiménez-Serra I, Puente-Sánchez F, Aguirre J. The emergence of interstellar molecular complexity explained by interacting networks. Proc Natl Acad Sci U S A 2022; 119:e2119734119. [PMID: 35867830 DOI: 10.1073/pnas.2119734119] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/24/2023] Open
Abstract
Recent years have witnessed the detection of an increasing number of complex organic molecules in interstellar space, some of them being of prebiotic interest. Disentangling the origin of interstellar prebiotic chemistry and its connection to biochemistry and ultimately, to biology is an enormously challenging scientific goal where the application of complexity theory and network science has not been fully exploited. Encouraged by this idea, we present a theoretical and computational framework to model the evolution of simple networked structures toward complexity. In our environment, complex networks represent simplified chemical compounds and interact optimizing the dynamical importance of their nodes. We describe the emergence of a transition from simple networks toward complexity when the parameter representing the environment reaches a critical value. Notably, although our system does not attempt to model the rules of real chemistry nor is dependent on external input data, the results describe the emergence of complexity in the evolution of chemical diversity in the interstellar medium. Furthermore, they reveal an as yet unknown relationship between the abundances of molecules in dark clouds and the potential number of chemical reactions that yield them as products, supporting the ability of the conceptual framework presented here to shed light on real scenarios. Our work reinforces the notion that some of the properties that condition the extremely complex journey from the chemistry in space to prebiotic chemistry and finally, to life could show relatively simple and universal patterns.
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199
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Abstract
Galaxy mergers provide a mechanism for galaxies to effectively funnel gas and materials toward their nuclei and fuel the central starbursts and accretion of supermassive black holes. In turn, the active nuclei drive galactic-scale outflows that subsequently impact the evolution of the host galaxies. The details of this transformative process as they pertain to the supermassive black holes remain ambiguous, partially due to the central obscuration commonly found in the dust-reddened merger hosts, and also because there are relatively few laboratories in the nearby universe where the process can be studied in depth. This review highlights the current state of the literature on the role of accreting supermassive black holes in local luminous infrared galaxies as seen from various windows within the electromagnetic spectrum. Specifically, we discuss the multiwavelength signatures of the active nucleus, its associated feeding and feedback processes, and the implications of multiple supermassive black holes found in nearby interacting galaxy systems for galaxy evolution from the observational perspective. We conclude with a future outlook on how the topic of active nuclei in low- and high-redshift galaxy mergers will benefit from the advent of next-generation observing facilities with unparalleled resolving power and sensitivity in the coming decade.
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200
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BASALGETE R, Torres-Díaz D, Lafosse A, Amiaud L, Féraud G, Jeseck P, Philippe L, Michaut X, Fillion JH, Bertin M. Indirect X-ray photodesorption of 15N 2 and 13CO from mixed and layered ices. J Chem Phys 2022; 157:084308. [DOI: 10.1063/5.0100014] [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: 11/15/2022] Open
Abstract
X-ray photodesorption yields of 15N2 and 13CO are derived as a function of the incident photon energy near the N (~ 400 eV) and O K-edge (~ 500 eV) for pure 15N2 ice and mixed 13CO:15N2 ices. The photodesorption spectra from the mixed ices reveal an indirect desorption mechanism for which the desorption of 15N2 and 13CO is triggered by the photo-absorption of respectively 13CO and 15N2. This mechanism is confirmed by the X-ray photodesorption of 13CO from a layered 13CO/15N2 ice irradiated at 401 eV, on the N 1s -> π* transition of 15N2. This latter experiment enables to quantify the relevant depth involved in the indirect desorption process, which is found to be 30 - 40 ML in that case. This value is further related to the energy transport of Auger electrons emitted from the photo-absorbing 15N2molecules that scatter towards the ice surface, inducing the desorption of 13CO. The photodesorption yields corrected from the energy that can participate to the desorption process (expressed in molecules desorbed by eV deposited) do not depend on the photon energy hence neither on the photo-absorbing molecule nor on its state after Auger decay. This demonstrates that X-ray induced electron stimulated desorption (XESD), mediated by Auger scattering, is the dominant process explaining the desorption of 15N2 and 13CO from the ices studied in this work.
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Affiliation(s)
| | | | - Anne Lafosse
- Chemistry Department, University Paris-Sud, France
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