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Wang H, Hu Z, Liu S, Zhang X, Sun Y, Dong F. Dissecting the Photochemical Reactivity of Metal Ions during Atmospheric Nitrate Transformations on Photoactive Mineral Dust. ENVIRONMENTAL SCIENCE & TECHNOLOGY 2024. [PMID: 38959497 DOI: 10.1021/acs.est.3c10192] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 07/05/2024]
Abstract
Dissecting the photochemical reactivity of metal ions is a significant contribution to understanding secondary pollutant formation, as they have a role to be reckoned with atmospheric chemistry. However, their photochemical reactivity has received limited attention within the active nitrogen cycle, particularly at the gas-solid interface. In this study, we delve into the contribution of magnesium ion (Mg2+) and ferric ion (Fe3+) to nitrate decomposition on the surface of photoactive mineral dust. Under simulated sunlight irradiation, the observed NOX production rate differs by an order of magnitude in the presence of Mg2+ (6.02 × 10-10 mol s-1) and Fe3+ (2.07 × 10-11 mol s-1). The markedly decreased fluorescence lifetime induced by Mg2+ and the change in the valence of Fe3+ revealed that Mg2+ and Fe3+ significantly affect the concentration of nitrate decomposition products by distinct photochemical reactivity with photogenerated electrons. Mg2+ promotes NOX production by accelerating charge transfer, while Fe3+ hinders nitrate decomposition by engaging in a redox cyclic reaction with Fe2+ to consume photogenerated carriers continuously. Furthermore, when Fe3+ coexists with other metal ions (e.g., Mg2+, Ca2+, Na+, and K+) and surpasses a proportion of approximately 12%, the photochemical reactivity of Fe3+ tends to be dominant in depleting photogenerated electrons and suppressing nitrate decomposition. Conversely, below this threshold, the released NOX concentration increases sharply as the proportion of Fe3+ decreases. This research offers valuable insights into the role of metal ions in nitrate transformation and the generation of reactive nitrogen species, contributing to a deep understanding of atmospheric photochemical reactions.
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Affiliation(s)
- Hong Wang
- Research Center for Carbon-Neutral Environmental & Energy Technology, Institute of Fundamental and Frontier Sciences, University of Electronic Science and Technology of China, Chengdu 611731, China
| | - Zehui Hu
- Research Center for Carbon-Neutral Environmental & Energy Technology, Institute of Fundamental and Frontier Sciences, University of Electronic Science and Technology of China, Chengdu 611731, China
| | - Shujun Liu
- School of Resources and Environment, University of Electronic Science and Technology of China, Chengdu 611731, China
| | - Xin Zhang
- Research Center for Carbon-Neutral Environmental & Energy Technology, Institute of Fundamental and Frontier Sciences, University of Electronic Science and Technology of China, Chengdu 611731, China
| | - Yanjuan Sun
- School of Resources and Environment, University of Electronic Science and Technology of China, Chengdu 611731, China
| | - Fan Dong
- Research Center for Carbon-Neutral Environmental & Energy Technology, Institute of Fundamental and Frontier Sciences, University of Electronic Science and Technology of China, Chengdu 611731, China
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2
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Owens A. A highly accurate potential energy surface for carbonyl sulphide (OCS): how important are the ab initio calculations? Phys Chem Chem Phys 2024; 26:17684-17694. [PMID: 38869020 DOI: 10.1039/d4cp01205d] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 06/14/2024]
Abstract
Ab initio quantum chemical methods can produce accurate molecular potential energy surfaces (PESs) capable of predicting the fundamental vibrational wavenumbers to within 1 cm-1. However, for high-resolution applications this is simply not good enough and empirical refinement is necessary, i.e. adjusting the PES to better match laboratory spectroscopic data. Here, the impact of the underlying ab initio calculations is rigorously investigated within the context of empirical refinement. For carbonyl sulphide (OCS), state-of-the-art electronic structure calculations are employed to construct higher- and lower-level ab initio PESs, which are then empirically refined in near-identical procedures. The initial ab initio calculations are shown to considerably affect the accuracy of the final refined PES, with an order-of-magnitude improvement in computed rotation-vibration energy levels achieved for OCS. In demonstrating this, the most accurate PES of the electronic ground state of OCS is produced, reproducing the fundamentals with a root-mean-square error (RMSE) of 0.004 cm-1, and 884 rovibrational energy levels below 14 000 cm-1 with an RMSE of 0.060 cm-1.
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Affiliation(s)
- Alec Owens
- Department of Physics and Astronomy, University College London, Gower Street, WC1E 6BT, London, UK.
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3
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Welbanks L, Bell TJ, Beatty TG, Line MR, Ohno K, Fortney JJ, Schlawin E, Greene TP, Rauscher E, McGill P, Murphy M, Parmentier V, Tang Y, Edelman I, Mukherjee S, Wiser LS, Lagage PO, Dyrek A, Arnold KE. A high internal heat flux and large core in a warm Neptune exoplanet. Nature 2024; 630:836-840. [PMID: 38768634 DOI: 10.1038/s41586-024-07514-w] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/15/2024] [Accepted: 05/02/2024] [Indexed: 05/22/2024]
Abstract
Interactions between exoplanetary atmospheres and internal properties have long been proposed to be drivers of the inflation mechanisms of gaseous planets and apparent atmospheric chemical disequilibrium conditions1. However, transmission spectra of exoplanets have been limited in their ability to observationally confirm these theories owing to the limited wavelength coverage of the Hubble Space Telescope (HST) and inferences of single molecules, mostly H2O (ref. 2). In this work, we present the panchromatic transmission spectrum of the approximately 750 K, low-density, Neptune-sized exoplanet WASP-107b using a combination of HST Wide Field Camera 3 (WFC3) and JWST Near-Infrared Camera (NIRCam) and Mid-Infrared Instrument (MIRI). From this spectrum, we detect spectroscopic features resulting from H2O (21σ), CH4 (5σ), CO (7σ), CO2 (29σ), SO2 (9σ) and NH3 (6σ). The presence of these molecules enables constraints on the atmospheric metal enrichment (M/H is 10-18× solar3), vertical mixing strength (log10Kzz = 8.4-9.0 cm2 s-1) and internal temperature (>345 K). The high internal temperature is suggestive of tidally driven inflation4 acting on a Neptune-like internal structure, which can naturally explain the large radius and low density of the planet. These findings suggest that eccentricity-driven tidal heating is a critical process governing atmospheric chemistry and interior-structure inferences for most of the cool (<1,000 K) super-Earth-to-Saturn-mass exoplanet population.
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Affiliation(s)
- Luis Welbanks
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA.
| | - Taylor J Bell
- Bay Area Environmental Research Institute, NASA's Ames Research Center, Moffett Field, CA, USA
- Space Science and Astrobiology Division, NASA's Ames Research Center, Moffett Field, CA, USA
| | - Thomas G Beatty
- Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA
| | - Michael R Line
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - Kazumasa Ohno
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
- Division of Science, National Astronomical Observatory of Japan (NAOJ), Tokyo, Japan
| | - Jonathan J Fortney
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | | | - Thomas P Greene
- Space Science and Astrobiology Division, NASA's Ames Research Center, Moffett Field, CA, USA
| | - Emily Rauscher
- Department of Astronomy, University of Michigan, Ann Arbor, MI, USA
| | - Peter McGill
- Space Science Institute, Lawrence Livermore National Laboratory, Livermore, CA, USA
| | - Matthew Murphy
- Steward Observatory, University of Arizona, Tucson, AZ, USA
| | - Vivien Parmentier
- Laboratoire Lagrange, Observatoire de la Côte d'Azur, Université Côte d'Azur, Nice, France
| | - Yao Tang
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Isaac Edelman
- Bay Area Environmental Research Institute, NASA's Ames Research Center, Moffett Field, CA, USA
| | - Sagnick Mukherjee
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Lindsey S Wiser
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - Pierre-Olivier Lagage
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | - Achrène Dyrek
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | - Kenneth E Arnold
- Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA
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4
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Sing DK, Rustamkulov Z, Thorngren DP, Barstow JK, Tremblin P, Alves de Oliveira C, Beck TL, Birkmann SM, Challener RC, Crouzet N, Espinoza N, Ferruit P, Giardino G, Gressier A, Lee EKH, Lewis NK, Maiolino R, Manjavacas E, Rauscher BJ, Sirianni M, Valenti JA. A warm Neptune's methane reveals core mass and vigorous atmospheric mixing. Nature 2024; 630:831-835. [PMID: 38768633 PMCID: PMC11208151 DOI: 10.1038/s41586-024-07395-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/18/2023] [Accepted: 04/05/2024] [Indexed: 05/22/2024]
Abstract
Observations of transiting gas giant exoplanets have revealed a pervasive depletion of methane1-4, which has only recently been identified atmospherically5,6. The depletion is thought to be maintained by disequilibrium processes such as photochemistry or mixing from a hotter interior7-9. However, the interiors are largely unconstrained along with the vertical mixing strength and only upper limits on the CH4 depletion have been available. The warm Neptune WASP-107b stands out among exoplanets with an unusually low density, reported low core mass10, and temperatures amenable to CH4, though previous observations have yet to find the molecule2,4. Here we present a JWST-NIRSpec transmission spectrum of WASP-107b that shows features from both SO2 and CH4 along with H2O, CO2, and CO. We detect methane with 4.2σ significance at an abundance of 1.0 ± 0.5 ppm, which is depleted by 3 orders of magnitude relative to equilibrium expectations. Our results are highly constraining for the atmosphere and interior, which indicate the envelope has a super-solar metallicity of 43 ± 8 × solar, a hot interior with an intrinsic temperature of Tint = 460 ± 40 K, and vigorous vertical mixing which depletes CH4 with a diffusion coefficient of Kzz = 1011.6±0.1 cm2 s-1. Photochemistry has a negligible effect on the CH4 abundance but is needed to account for the SO2. We infer a core mass of11.5 - 3.6 + 3.0 M ⊕ , which is much higher than previous upper limits10, releasing a tension with core-accretion models11.
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Affiliation(s)
- David K Sing
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA.
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA.
| | - Zafar Rustamkulov
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA
| | - Daniel P Thorngren
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | - Joanna K Barstow
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | - Pascal Tremblin
- Université Paris-Saclay, UVSQ, CNRS, CEA, Maison de la Simulation, Gif-sur-Yvette, France
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | | | - Tracy L Beck
- Space Telescope Science Institute, Baltimore, MD, USA
| | | | - Ryan C Challener
- Department of Astronomy and Carl Sagan Institute, Cornell University, Ithaca, NY, USA
| | - Nicolas Crouzet
- Leiden Observatory, Leiden University, Leiden, The Netherlands
| | | | - Pierre Ferruit
- European Space Agency, European Space Astronomy Centre, Madrid, Spain
| | - Giovanna Giardino
- ATG Europe for the European Space Agency, ESTEC, Noordwijk, The Netherlands
| | | | - Elspeth K H Lee
- Center for Space and Habitability, University of Bern, Bern, Switzerland
| | - Nikole K Lewis
- Department of Astronomy and Carl Sagan Institute, Cornell University, Ithaca, NY, USA
| | | | - Elena Manjavacas
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
- AURA for the European Space Agency (ESA), Space Telescope Science Institute, Baltimore, MD, USA
| | | | - Marco Sirianni
- European Space Agency (ESA) Office, Space Telescope Science Institute, Baltimore, MD, USA
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5
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Luo Z, Wu Y, Yang S, Li Z, Hua W, Chen Z, Che L, Wang X, Ashfold MNR, Yuan K. Unraveling the Rich Fragmentation Dynamics Associated with S-H Bond Fission Following Photoexcitation of H 2S at Wavelengths ∼129.1 nm. J Phys Chem A 2024; 128:3351-3360. [PMID: 38651288 DOI: 10.1021/acs.jpca.4c01478] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/25/2024]
Abstract
H2S is being detected in the atmospheres of ever more interstellar bodies, and photolysis is an important mechanism by which it is processed. Here, we report H Rydberg atom time-of-flight measurements following the excitation of H2S molecules to selected rotational (JKaKc') levels of the 1B1 Rydberg state associated with the strong absorption feature at wavelengths of λ ∼ 129.1 nm. Analysis of the total kinetic energy release spectra derived from these data reveals that all levels predissociate to yield H atoms in conjunction with both SH(A) and SH(X) partners and that the primary SH(A)/SH(X) product branching ratio increases steeply with ⟨Jb2⟩, the square of the rotational angular momentum about the b-inertial axis in the excited state. These products arise via competing homogeneous (vibronic) and heterogeneous (Coriolis-induced) predissociation pathways that involve coupling to dissociative potential energy surfaces (PES(s)) of, respectively, 1A″ and 1A' symmetries. The present data also show H + SH(A) product formation when exciting the JKaKc' = 000 and 111 levels, for which ⟨Jb2⟩ = 0 and Coriolis coupling to the 1A' PES(s) is symmetry forbidden, implying the operation of another, hitherto unrecognized, route to forming H + SH(A) products following excitation of H2S at energies above ∼9 eV. These data can be expected to stimulate future ab initio molecular dynamic studies that test, refine, and define the currently inferred predissociation pathways available to photoexcited H2S molecules.
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Affiliation(s)
- Zijie Luo
- Marine Engineering College, Dalian Maritime University, Liaoning 116026, China
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
| | - Yucheng Wu
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - Shuaikang Yang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
- Department of Chemical Physics, School of Chemistry and Materials Science, University of Science and Technology of China, Jinzhai Road 96, Hefei, Anhui 230026, China
| | - Zhenxing Li
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
| | - Wei Hua
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
| | - Zhichao Chen
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
| | - Li Che
- Department of Physics, School of Science, Dalian Maritime University, Dalian 116026, China
| | - Xingan Wang
- Department of Chemical Physics, School of Chemistry and Materials Science, University of Science and Technology of China, Jinzhai Road 96, Hefei, Anhui 230026, China
| | | | - Kaijun Yuan
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, China
- University of Chinese Academy of Sciences, Beijing 100049, China
- Hefei National Laboratory, Hefei 230088, China
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6
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Powell D, Feinstein AD, Lee EKH, Zhang M, Tsai SM, Taylor J, Kirk J, Bell T, Barstow JK, Gao P, Bean JL, Blecic J, Chubb KL, Crossfield IJM, Jordan S, Kitzmann D, Moran SE, Morello G, Moses JI, Welbanks L, Yang J, Zhang X, Ahrer EM, Bello-Arufe A, Brande J, Casewell SL, Crouzet N, Cubillos PE, Demory BO, Dyrek A, Flagg L, Hu R, Inglis J, Jones KD, Kreidberg L, López-Morales M, Lagage PO, Meier Valdés EA, Miguel Y, Parmentier V, Piette AAA, Rackham BV, Radica M, Redfield S, Stevenson KB, Wakeford HR, Aggarwal K, Alam MK, Batalha NM, Batalha NE, Benneke B, Berta-Thompson ZK, Brady RP, Caceres C, Carter AL, Désert JM, Harrington J, Iro N, Line MR, Lothringer JD, MacDonald RJ, Mancini L, Molaverdikhani K, Mukherjee S, Nixon MC, Oza AV, Palle E, Rustamkulov Z, Sing DK, Steinrueck ME, Venot O, Wheatley PJ, Yurchenko SN. Sulfur dioxide in the mid-infrared transmission spectrum of WASP-39b. Nature 2024; 626:979-983. [PMID: 38232945 PMCID: PMC10901732 DOI: 10.1038/s41586-024-07040-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/11/2023] [Accepted: 01/05/2024] [Indexed: 01/19/2024]
Abstract
The recent inference of sulfur dioxide (SO2) in the atmosphere of the hot (approximately 1,100 K), Saturn-mass exoplanet WASP-39b from near-infrared JWST observations1-3 suggests that photochemistry is a key process in high-temperature exoplanet atmospheres4. This is because of the low (<1 ppb) abundance of SO2 under thermochemical equilibrium compared with that produced from the photochemistry of H2O and H2S (1-10 ppm)4-9. However, the SO2 inference was made from a single, small molecular feature in the transmission spectrum of WASP-39b at 4.05 μm and, therefore, the detection of other SO2 absorption bands at different wavelengths is needed to better constrain the SO2 abundance. Here we report the detection of SO2 spectral features at 7.7 and 8.5 μm in the 5-12-μm transmission spectrum of WASP-39b measured by the JWST Mid-Infrared Instrument (MIRI) Low Resolution Spectrometer (LRS)10. Our observations suggest an abundance of SO2 of 0.5-25 ppm (1σ range), consistent with previous findings4. As well as SO2, we find broad water-vapour absorption features, as well as an unexplained decrease in the transit depth at wavelengths longer than 10 μm. Fitting the spectrum with a grid of atmospheric forward models, we derive an atmospheric heavy-element content (metallicity) for WASP-39b of approximately 7.1-8.0 times solar and demonstrate that photochemistry shapes the spectra of WASP-39b across a broad wavelength range.
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Affiliation(s)
- Diana Powell
- Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA.
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA.
| | - Adina D Feinstein
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO, USA
| | - Elspeth K H Lee
- Center for Space and Habitability, University of Bern, Bern, Switzerland
| | - Michael Zhang
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - Shang-Min Tsai
- Department of Earth Sciences, University of California, Riverside, Riverside, CA, USA
| | - Jake Taylor
- Department of Physics, University of Oxford, Oxford, UK
- Institut Trottier de Recherche sur les Exoplanètes, Université de Montréal, Montréal, Quebec, Canada
- Département de Physique, Université de Montréal, Montréal, Quebec, Canada
| | - James Kirk
- Department of Physics, Imperial College London, London, UK
| | - Taylor Bell
- Bay Area Environmental Research Institute, NASA Ames Research Center, Moffett Field, CA, USA
- Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, CA, USA
| | - Joanna K Barstow
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | - Peter Gao
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Jacob L Bean
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - Jasmina Blecic
- Department of Physics, New York University Abu Dhabi, Abu Dhabi, United Arab Emirates
- Center for Astro, Particle, and Planetary Physics (CAP3), New York University Abu Dhabi, Abu Dhabi, United Arab Emirates
| | - Katy L Chubb
- Centre for Exoplanet Science, University of St Andrews, St Andrews, UK
| | - Ian J M Crossfield
- Department of Physics & Astronomy, University of Kansas, Lawrence, KS, USA
| | - Sean Jordan
- Institute of Astronomy, University of Cambridge, Cambridge, UK
| | - Daniel Kitzmann
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO, USA
| | - Sarah E Moran
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - Giuseppe Morello
- Department of Space, Earth and Environment, Chalmers University of Technology, Gothenburg, Sweden
- Instituto de Astrofísica de Canarias (IAC), Tenerife, Spain
- INAF - Palermo Astronomical Observatory, Palermo, Italy
| | | | - Luis Welbanks
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - Jeehyun Yang
- Planetary Sciences Section, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Xi Zhang
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Eva-Maria Ahrer
- Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK
- Department of Physics, University of Warwick, Coventry, UK
| | - Aaron Bello-Arufe
- Astrophysics Section, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Jonathan Brande
- Department of Physics & Astronomy, University of Kansas, Lawrence, KS, USA
| | - S L Casewell
- School of Physics and Astronomy, University of Leicester, Leicester, UK
| | - Nicolas Crouzet
- Leiden Observatory, University of Leiden, Leiden, The Netherlands
| | - Patricio E Cubillos
- INAF - Turin Astrophysical Observatory, Pino Torinese, Italy
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Brice-Olivier Demory
- Center for Space and Habitability, University of Bern, Bern, Switzerland
- Space and Planetary Sciences, Institute of Physics, University of Bern, Bern, Switzerland
| | - Achrène Dyrek
- Université Paris-Saclay, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | - Laura Flagg
- Department of Astronomy, Cornell University, Ithaca, NY, USA
- Carl Sagan Institute, Cornell University, Ithaca, NY, USA
| | - Renyu Hu
- Astrophysics Section, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Julie Inglis
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Kathryn D Jones
- Center for Space and Habitability, University of Bern, Bern, Switzerland
| | | | | | | | | | - Yamila Miguel
- Leiden Observatory, University of Leiden, Leiden, The Netherlands
- SRON Netherlands Institute for Space Research, Leiden, The Netherlands
| | - Vivien Parmentier
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, French Riviera, France
| | - Anjali A A Piette
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Benjamin V Rackham
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Michael Radica
- Institut Trottier de Recherche sur les Exoplanètes, Université de Montréal, Montréal, Quebec, Canada
- Département de Physique, Université de Montréal, Montréal, Quebec, Canada
| | - Seth Redfield
- Astronomy Department, Wesleyan University, Middletown, CT, USA
- Van Vleck Observatory, Wesleyan University, Middletown, CT, USA
| | - Kevin B Stevenson
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | | | | | - Munazza K Alam
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Natalie M Batalha
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | | | - Björn Benneke
- Institut Trottier de Recherche sur les Exoplanètes, Université de Montréal, Montréal, Quebec, Canada
- Département de Physique, Université de Montréal, Montréal, Quebec, Canada
| | - Zach K Berta-Thompson
- Department of Astrophysical and Planetary Sciences, University of Colorado Boulder, Boulder, CO, USA
| | - Ryan P Brady
- Department of Physics and Astronomy, University College London, London, UK
| | - Claudio Caceres
- Instituto de Astrofisica, Facultad Ciencias Exactas, Universidad Andres Bello, Santiago, Chile
- Centro de Astrofisica y Tecnologias Afines (CATA), Santiago, Chile
- Núcleo Milenio de Formación Planetaria (NPF), Valparaíso, Chile
| | - Aarynn L Carter
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Jean-Michel Désert
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands
| | - Joseph Harrington
- Planetary Sciences Group, Department of Physics and Florida Space Institute, University of Central Florida, Orlando, FL, USA
| | - Nicolas Iro
- Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany
| | - Michael R Line
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | | | - Ryan J MacDonald
- Department of Astronomy, University of Michigan, Ann Arbor, MI, USA
| | - Luigi Mancini
- INAF - Turin Astrophysical Observatory, Pino Torinese, Italy
- Max Planck Institute for Astronomy, Heidelberg, Germany
- Department of Physics, University of Rome "Tor Vergata", Rome, Italy
| | - Karan Molaverdikhani
- Universitäts-Sternwarte, Ludwig-Maximilians-Universität München, München, Germany
- Exzellenzcluster Origins, Garching, Germany
| | - Sagnick Mukherjee
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Matthew C Nixon
- Department of Astronomy, University of Maryland, College Park, MD, USA
| | - Apurva V Oza
- Astrophysics Section, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Enric Palle
- Instituto de Astrofísica de Canarias (IAC), Tenerife, Spain
| | - Zafar Rustamkulov
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA
| | - David K Sing
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | | | - Olivia Venot
- Université de Paris Cité and Université Paris-Est Creteil, CNRS, LISA, Paris, France
| | - Peter J Wheatley
- Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK
- Department of Physics, University of Warwick, Coventry, UK
| | - Sergei N Yurchenko
- Department of Physics and Astronomy, University College London, London, UK
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7
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Dyrek A, Min M, Decin L, Bouwman J, Crouzet N, Mollière P, Lagage PO, Konings T, Tremblin P, Güdel M, Pye J, Waters R, Henning T, Vandenbussche B, Ardevol Martinez F, Argyriou I, Ducrot E, Heinke L, van Looveren G, Absil O, Barrado D, Baudoz P, Boccaletti A, Cossou C, Coulais A, Edwards B, Gastaud R, Glasse A, Glauser A, Greene TP, Kendrew S, Krause O, Lahuis F, Mueller M, Olofsson G, Patapis P, Rouan D, Royer P, Scheithauer S, Waldmann I, Whiteford N, Colina L, van Dishoeck EF, Östlin G, Ray TP, Wright G. SO 2, silicate clouds, but no CH 4 detected in a warm Neptune. Nature 2024; 625:51-54. [PMID: 37967578 DOI: 10.1038/s41586-023-06849-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/23/2023] [Accepted: 11/08/2023] [Indexed: 11/17/2023]
Abstract
WASP-107b is a warm (approximately 740 K) transiting planet with a Neptune-like mass of roughly 30.5 M⊕ and Jupiter-like radius of about 0.94 RJ (refs. 1,2), whose extended atmosphere is eroding3. Previous observations showed evidence for water vapour and a thick, high-altitude condensate layer in the atmosphere of WASP-107b (refs. 4,5). Recently, photochemically produced sulfur dioxide (SO2) was detected in the atmosphere of a hot (about 1,200 K) Saturn-mass planet from transmission spectroscopy near 4.05 μm (refs. 6,7), but for temperatures below about 1,000 K, sulfur is predicted to preferably form sulfur allotropes instead of SO2 (refs. 8-10). Here we report the 9σ detection of two fundamental vibration bands of SO2, at 7.35 μm and 8.69 μm, in the transmission spectrum of WASP-107b using the Mid-Infrared Instrument (MIRI) of JWST. This discovery establishes WASP-107b as the second irradiated exoplanet with confirmed photochemistry, extending the temperature range of exoplanets exhibiting detected photochemistry from about 1,200 K down to about 740 K. Furthermore, our spectral analysis reveals the presence of silicate clouds, which are strongly favoured (around 7σ) over simpler cloud set-ups. Furthermore, water is detected (around 12σ) but methane is not. These findings provide evidence of disequilibrium chemistry and indicate a dynamically active atmosphere with a super-solar metallicity.
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Affiliation(s)
- Achrène Dyrek
- Université Paris Cité, Université Paris-Saclay, CEA, CNRS, AIM, Gif-sur-Yvette, France.
| | - Michiel Min
- SRON Netherlands Institute for Space Research, Leiden, The Netherlands
| | - Leen Decin
- Institute of Astronomy, KU Leuven, Leuven, Belgium
| | - Jeroen Bouwman
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - Nicolas Crouzet
- Leiden Observatory, Leiden University, Leiden, The Netherlands
| | - Paul Mollière
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - Pierre-Olivier Lagage
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | | | - Pascal Tremblin
- Université Paris-Saclay, UVSQ, CNRS, CEA, Maison de la Simulation, Gif-sur-Yvette, France
| | - Manuel Güdel
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
- Department of Astrophysics, University of Vienna, Vienna, Austria
- Institute for Particle Physics and Astrophysics, ETH Zürich, Zürich, Switzerland
| | - John Pye
- Space Research Centre, School of Physics & Astronomy, University of Leicester, Leicester, UK
| | - Rens Waters
- SRON Netherlands Institute for Space Research, Leiden, The Netherlands
- Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands
- HFML-FELIX, Radboud University, Nijmegen, The Netherlands
| | - Thomas Henning
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | | | - Francisco Ardevol Martinez
- SRON Netherlands Institute for Space Research, Leiden, The Netherlands
- Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
- Centre for Exoplanet Science, University of Edinburgh, Edinburgh, UK
- School of GeoSciences, University of Edinburgh, Edinburgh, UK
| | | | - Elsa Ducrot
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
| | - Linus Heinke
- Institute of Astronomy, KU Leuven, Leuven, Belgium
- Centre for Exoplanet Science, University of Edinburgh, Edinburgh, UK
- School of GeoSciences, University of Edinburgh, Edinburgh, UK
| | | | | | - David Barrado
- Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain
| | - Pierre Baudoz
- LESIA, Observatoire de Paris, CNRS, Université Paris Cité, Sorbonne Université, Meudon, France
| | - Anthony Boccaletti
- LESIA, Observatoire de Paris, CNRS, Université Paris Cité, Sorbonne Université, Meudon, France
| | - Christophe Cossou
- Département d'Electronique des Détecteurs et d'Informatique pour la Physique, Université Paris-Saclay, CEA, Gif-sur-Yvette, France
| | - Alain Coulais
- Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, Gif-sur-Yvette, France
- LERMA, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS, Paris, France
| | - Billy Edwards
- SRON Netherlands Institute for Space Research, Leiden, The Netherlands
| | - René Gastaud
- Département d'Electronique des Détecteurs et d'Informatique pour la Physique, Université Paris-Saclay, CEA, Gif-sur-Yvette, France
| | - Alistair Glasse
- UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK
| | - Adrian Glauser
- Institute for Particle Physics and Astrophysics, ETH Zürich, Zürich, Switzerland
| | - Thomas P Greene
- Space Science and Astrobiology Division, NASA's Ames Research Center, Moffett Field, CA, USA
| | - Sarah Kendrew
- European Space Agency, Space Telescope Science Institute, Baltimore, MD, USA
| | - Oliver Krause
- Max-Planck-Institut für Astronomie (MPIA), Heidelberg, Germany
| | - Fred Lahuis
- SRON Netherlands Institute for Space Research, Leiden, The Netherlands
| | - Michael Mueller
- Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
| | - Goran Olofsson
- Department of Astronomy, Stockholm University, AlbaNova University Center, Stockholm, Sweden
| | - Polychronis Patapis
- Institute for Particle Physics and Astrophysics, ETH Zürich, Zürich, Switzerland
| | - Daniel Rouan
- Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain
| | - Pierre Royer
- Institute of Astronomy, KU Leuven, Leuven, Belgium
| | | | - Ingo Waldmann
- Department of Physics and Astronomy, University College London, London, UK
| | - Niall Whiteford
- Department of Astrophysics, American Museum of Natural History, New York, NY, USA
| | - Luis Colina
- Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain
| | | | - Göran Östlin
- Université Paris Cité, Université Paris-Saclay, CEA, CNRS, AIM, Gif-sur-Yvette, France
- Department of Astronomy, Oskar Klein Centre, Stockholm University, Stockholm, Sweden
| | - Tom P Ray
- School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, Ireland
| | - Gillian Wright
- UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK
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Bell TJ, Welbanks L, Schlawin E, Line MR, Fortney JJ, Greene TP, Ohno K, Parmentier V, Rauscher E, Beatty TG, Mukherjee S, Wiser LS, Boyer ML, Rieke MJ, Stansberry JA. Methane throughout the atmosphere of the warm exoplanet WASP-80b. Nature 2023; 623:709-712. [PMID: 37993572 DOI: 10.1038/s41586-023-06687-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/21/2023] [Accepted: 09/27/2023] [Indexed: 11/24/2023]
Abstract
The abundances of main carbon- and oxygen-bearing gases in the atmospheres of giant exoplanets provide insights into atmospheric chemistry and planet formation processes1,2. Thermochemistry suggests that methane (CH4) should be the dominant carbon-bearing species below about 1,000 K over a range of plausible atmospheric compositions3; this is the case for the solar system planets4 and has been confirmed in the atmospheres of brown dwarfs and self-luminous, directly imaged exoplanets5. However, CH4 has not yet been definitively detected with space-based spectroscopy in the atmosphere of a transiting exoplanet6-11, but a few detections have been made with ground-based, high-resolution transit spectroscopy12,13 including a tentative detection for WASP-80b (ref. 14). Here we report transmission and emission spectra spanning 2.4-4.0 μm of the 825 K warm Jupiter WASP-80b taken with the NIRCam instrument of the JWST, both of which show strong evidence of CH4 at greater than 6σ significance. The derived CH4 abundances from both viewing geometries are consistent with each other and with solar to sub-solar C/O and around five times solar metallicity, which is consistent with theoretical predictions15-17.
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Affiliation(s)
- Taylor J Bell
- Bay Area Environmental Research Institute, NASA Ames Research Center, Moffett Field, CA, USA.
- Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, CA, USA.
| | - Luis Welbanks
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | | | - Michael R Line
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - Jonathan J Fortney
- Department of Astronomy and Astrophysics, University of California Santa Cruz, Santa Cruz, CA, USA
| | - Thomas P Greene
- Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, CA, USA
| | - Kazumasa Ohno
- Department of Astronomy and Astrophysics, University of California Santa Cruz, Santa Cruz, CA, USA
- Division of Science, National Astronomical Observatory of Japan, Tokyo, Japan
| | - Vivien Parmentier
- Laboratoire Lagrange, Observatoire de la Côte d'Azur, Université Côte d'Azur, Nice, France
| | - Emily Rauscher
- Department of Astronomy, University of Michigan, Ann Arbor, MI, USA
| | - Thomas G Beatty
- Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA
| | - Sagnick Mukherjee
- Department of Astronomy and Astrophysics, University of California Santa Cruz, Santa Cruz, CA, USA
| | - Lindsey S Wiser
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | | | - Marcia J Rieke
- Steward Observatory, University of Arizona, Tucson, AZ, USA
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9
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Zhang X. JWST's eyes on an alien world. Innovation (N Y) 2023; 4:100428. [PMID: 37206619 PMCID: PMC10189546 DOI: 10.1016/j.xinn.2023.100428] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/09/2023] [Accepted: 04/18/2023] [Indexed: 05/21/2023] Open
Affiliation(s)
- Xi Zhang
- Department of Earth and Planetary Sciences, University of California Santa Cruz, Santa Cruz, CA 95064, USA
- Corresponding author
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