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  1. AU="Amundsen, David S"
  2. AU="Konios, Dimitrios"
  3. AU="Lindh, Ingrid"
  4. AU=Zhao Chunyan
  5. AU="Scalia, Jennifer B"
  6. AU="Balint, Lajos"
  7. AU="Liang, Siping"
  8. AU="Wong, Anthony"
  9. AU="Müjdat YENİCESU"
  10. AU="Brooks, M L"
  11. AU="Garcia-Gutierrez, Ania" AU="Garcia-Gutierrez, Ania"
  12. AU="Marina Paola Gardiman"
  13. AU="Labarthe, Simon"
  14. AU="Jiahui Li"
  15. AU="Geier, Johannes"
  16. AU=Thangaraju Pugazhenthan
  17. AU="Tapio, Joona"
  18. AU="Navaratnam, Dhasakumar"
  19. AU="Blank, Marissa Cathleen"
  20. AU="Sadeghi, Yasaman"
  21. AU=Ye Keqiang
  22. AU="Huda, Walter"
  23. AU="Petrova, Polina E"
  24. AU="Pond, Gregory"
  25. AU=Krzewski Konrad
  26. AU="Feng, Yuquan"
  27. AU="Schmermund, Ben Niklas"
  28. AU="Soni, Payal D"
  29. AU="Romero-García, Carolina"
  30. AU="Petty, Lloyd"
  31. AU="James E. Posey"

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  1. Artikel: A hybrid line list for CH

    Yurchenko, Sergei N / Amundsen, David S / Tennyson, Jonathan / Waldmann, Ingo P

    Astronomy and astrophysics

    2017  Band 605

    Abstract: Aims: Molecular line lists (a catalogue of transition frequencies and line strengths) are important for modelling absorption and emission processes in atmospheres of different astronomical objects, such as cool stars and exoplanets. In order to be ... ...

    Abstract Aims: Molecular line lists (a catalogue of transition frequencies and line strengths) are important for modelling absorption and emission processes in atmospheres of different astronomical objects, such as cool stars and exoplanets. In order to be applicable for high temperatures, line lists for molecules like methane must contain billions of transitions, which makes their direct (line-by-line usage) application in radiative transfer calculations impracticable. Here we suggest a new, hybrid line list format to mitigate this problem, based on the idea of temperature-dependent absorption continuum.
    Methods: The line list is partitioned into a large set of relatively weak lines and a small set of important, stronger lines. The weaker lines are then used either to construct a temperature-dependent (but pressure-independent) set of intensity cross sections or are blended into a greatly reduced set of 'super-lines'. The strong lines are kept in the form of temperature-independent Einstein
    Results: A line list for methane (CH
    Sprache Englisch
    Erscheinungsdatum 2017-08-18
    Erscheinungsland Germany
    Dokumenttyp Journal Article
    ZDB-ID 1458466-9
    ISSN 1432-0746 ; 0004-6361
    ISSN (online) 1432-0746
    ISSN 0004-6361
    DOI 10.1051/0004-6361/201731026
    Datenquelle MEDical Literature Analysis and Retrieval System OnLINE

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  2. Artikel ; Online: Habitable Climate Scenarios for Proxima Centauri b with a Dynamic Ocean.

    Del Genio, Anthony D / Way, Michael J / Amundsen, David S / Aleinov, Igor / Kelley, Maxwell / Kiang, Nancy Y / Clune, Thomas L

    Astrobiology

    2018  Band 19, Heft 1, Seite(n) 99–125

    Abstract: The nearby exoplanet Proxima Centauri b will be a prime future target for characterization, despite questions about its retention of water. Climate models with static oceans suggest that Proxima b could harbor a small dayside surface ocean despite its ... ...

    Abstract The nearby exoplanet Proxima Centauri b will be a prime future target for characterization, despite questions about its retention of water. Climate models with static oceans suggest that Proxima b could harbor a small dayside surface ocean despite its weak instellation. We present the first climate simulations of Proxima b with a dynamic ocean. We find that an ocean-covered Proxima b could have a much broader area of surface liquid water but at much colder temperatures than previously suggested, due to ocean heat transport and/or depression of the freezing point by salinity. Elevated greenhouse gas concentrations do not necessarily produce more open ocean because of dynamical regime transitions between a state with an equatorial Rossby-Kelvin wave pattern and a state with a day-night circulation. For an evolutionary path leading to a highly saline ocean, Proxima b could be an inhabited, mostly open ocean planet with halophilic life. A freshwater ocean produces a smaller liquid region than does an Earth salinity ocean. An ocean planet in 3:2 spin-orbit resonance has a permanent tropical waterbelt for moderate eccentricity. A larger versus smaller area of surface liquid water for similar equilibrium temperature may be distinguishable by using the amplitude of the thermal phase curve. Simulations of Proxima Centauri b may be a model for the habitability of weakly irradiated planets orbiting slightly cooler or warmer stars, for example, in the TRAPPIST-1, LHS 1140, GJ 273, and GJ 3293 systems.
    Mesh-Begriff(e) Atmosphere ; Climate ; Exobiology ; Greenhouse Gases ; Models, Theoretical ; Oceans and Seas ; Planets ; Water Movements
    Chemische Substanzen Greenhouse Gases
    Sprache Englisch
    Erscheinungsdatum 2018-09-05
    Erscheinungsland United States
    Dokumenttyp Journal Article ; Research Support, U.S. Gov't, Non-P.H.S.
    ZDB-ID 2047736-3
    ISSN 1557-8070 ; 1531-1074
    ISSN (online) 1557-8070
    ISSN 1531-1074
    DOI 10.1089/ast.2017.1760
    Datenquelle MEDical Literature Analysis and Retrieval System OnLINE

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  3. Artikel: Albedos, Equilibrium Temperatures, and Surface Temperatures of Habitable Planets.

    Del Genio, Anthony D / Kiang, Nancy Y / Way, Michael J / Amundsen, David S / Sohl, Linda E / Fujii, Yuka / Chandler, Mark / Aleinov, Igor / Colose, Christopher M / Guzewich, Scott D / Kelley, Maxwell

    The Astrophysical journal

    2019  Band 884, Heft 1

    Abstract: The potential habitability of known exoplanets is often categorized by a nominal equilibrium temperature assuming a Bond albedo of either ∼0.3, similar to Earth, or 0. As an indicator of habitability, this leaves much to be desired, because albedos of ... ...

    Abstract The potential habitability of known exoplanets is often categorized by a nominal equilibrium temperature assuming a Bond albedo of either ∼0.3, similar to Earth, or 0. As an indicator of habitability, this leaves much to be desired, because albedos of other planets can be very different, and because surface temperature exceeds equilibrium temperature due to the atmospheric greenhouse effect. We use an ensemble of general circulation model simulations to show that for a range of habitable planets, much of the variability of Bond albedo, equilibrium temperature and even surface temperature can be predicted with useful accuracy from incident stellar flux and stellar temperature, two known parameters for every confirmed exoplanet. Earth's Bond albedo is near the minimum possible for habitable planets orbiting G stars, because of increasing contributions from clouds and sea ice/snow at higher and lower instellations, respectively. For habitable M star planets, Bond albedo is usually lower than Earth's because of near-IR H
    Sprache Englisch
    Erscheinungsdatum 2019-10-14
    Erscheinungsland United States
    Dokumenttyp Journal Article
    ZDB-ID 2960-9
    ISSN 0004-637X
    ISSN 0004-637X
    DOI 10.3847/1538-4357/ab3be8
    Datenquelle MEDical Literature Analysis and Retrieval System OnLINE

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  4. Artikel ; Online: HAT-P-26b: A Neptune-mass exoplanet with a well-constrained heavy element abundance.

    Wakeford, Hannah R / Sing, David K / Kataria, Tiffany / Deming, Drake / Nikolov, Nikolay / Lopez, Eric D / Tremblin, Pascal / Amundsen, David S / Lewis, Nikole K / Mandell, Avi M / Fortney, Jonathan J / Knutson, Heather / Benneke, Björn / Evans, Thomas M

    Science (New York, N.Y.)

    2017  Band 356, Heft 6338, Seite(n) 628–631

    Abstract: A correlation between giant-planet mass and atmospheric heavy elemental abundance was first noted in the past century from observations of planets in our own Solar System and has served as a cornerstone of planet-formation theory. Using data from the ... ...

    Abstract A correlation between giant-planet mass and atmospheric heavy elemental abundance was first noted in the past century from observations of planets in our own Solar System and has served as a cornerstone of planet-formation theory. Using data from the Hubble and Spitzer Space Telescopes from 0.5 to 5 micrometers, we conducted a detailed atmospheric study of the transiting Neptune-mass exoplanet HAT-P-26b. We detected prominent H
    Sprache Englisch
    Erscheinungsdatum 2017--12
    Erscheinungsland United States
    Dokumenttyp Journal Article ; Research Support, Non-U.S. Gov't
    ZDB-ID 128410-1
    ISSN 1095-9203 ; 0036-8075
    ISSN (online) 1095-9203
    ISSN 0036-8075
    DOI 10.1126/science.aah4668
    Datenquelle MEDical Literature Analysis and Retrieval System OnLINE

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  5. Buch ; Online: The Effects of Consistent Chemical Kinetics Calculations on the Pressure-Temperature Profiles and Emission Spectra of Hot Jupiters

    Drummond, Benjamin / Tremblin, Pascal / Baraffe, Isabelle / Amundsen, David S. / Mayne, Nathan J. / Venot, Olivia / Goyal, Jayesh

    2016  

    Abstract: In this work we investigate the impact of calculating non-equilibrium chemical abundances consistently with the temperature structure for the atmospheres of highly-irradiated, close-in gas giant exoplanets. Chemical kinetics models have been widely used ... ...

    Abstract In this work we investigate the impact of calculating non-equilibrium chemical abundances consistently with the temperature structure for the atmospheres of highly-irradiated, close-in gas giant exoplanets. Chemical kinetics models have been widely used in the literature to investigate the chemical compositions of hot Jupiter atmospheres which are expected to be driven away from chemical equilibrium via processes such as vertical mixing and photochemistry. All of these models have so far used pressure--temperature (P-T) profiles as fixed model input. This results in a decoupling of the chemistry from the radiative and thermal properties of the atmosphere, despite the fact that in nature they are intricately linked. We use a one-dimensional radiative-convective equilibrium model, ATMO, which includes a sophisticated chemistry scheme to calculate P-T profiles which are fully consistent with non-equilibrium chemical abundances, including vertical mixing and photochemistry. Our primary conclusion is that, in cases of strong chemical disequilibrium, consistent calculations can lead to differences in the P-T profile of up to 100 K compared to the P-T profile derived assuming chemical equilibrium. This temperature change can, in turn, have important consequences for the chemical abundances themselves as well as for the simulated emission spectra. In particular, we find that performing the chemical kinetics calculation consistently can reduce the overall impact of non-equilibrium chemistry on the observable emission spectrum of hot Jupiters. Simulated observations derived from non-consistent models could thus yield the wrong interpretation. We show that this behaviour is due to the non-consistent models violating the energy budget balance of the atmosphere.

    Comment: 16 pages, 26 figures, accepted in A&A
    Schlagwörter Astrophysics - Earth and Planetary Astrophysics
    Thema/Rubrik (Code) 660
    Erscheinungsdatum 2016-07-14
    Erscheinungsland us
    Dokumenttyp Buch ; Online
    Datenquelle BASE - Bielefeld Academic Search Engine (Lebenswissenschaftliche Auswahl)

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  6. Artikel ; Online: HAT-P-26b

    Wakeford, Hannah R. / Sing, David K. / Kataria, Tiffany / Deming, Drake / Nikolov, Nikolay / Lopez, Eric D. / Tremblin, Pascal / Amundsen, David S. / Lewis, Nikole K. / Mandell, Avi M. / Fortney, Jonathan J. / Knutson, Heather / Benneke, Björn / Evans, Thomas M.

    Science

    A Neptune-mass exoplanet with a well-constrained heavy element abundance

    2017  Band 356, Heft 6338, Seite(n) 628–631

    Abstract: How much water is in that exoplanet? Thousands of exoplanets have been identified, but little is known about their atmospheres, especially for bodies smaller than Jupiter. The extent and composition of an atmosphere can provide evidence for how an ... ...

    Abstract How much water is in that exoplanet? Thousands of exoplanets have been identified, but little is known about their atmospheres, especially for bodies smaller than Jupiter. The extent and composition of an atmosphere can provide evidence for how an exoplanet formed. Wakeford et al. used the Hubble and Spitzer space telescopes to measure the spectrum of the atmosphere around HAT-P-26b, a Neptune-sized exoplanet discovered in 2011. They detected signatures of water and clouds; this allowed them to constrain the atmospheric composition, which appears not to have been altered substantially since it formed. Science , this issue p. 628
    Schlagwörter Multidisciplinary
    Sprache Englisch
    Verlag American Association for the Advancement of Science (AAAS)
    Erscheinungsland us
    Dokumenttyp Artikel ; Online
    ZDB-ID 128410-1
    ISSN 1095-9203 ; 0036-8075
    ISSN (online) 1095-9203
    ISSN 0036-8075
    DOI 10.1126/science.aah4668
    Datenquelle BASE - Bielefeld Academic Search Engine (Lebenswissenschaftliche Auswahl)

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  7. Artikel ; Online: An ultrahot gas-giant exoplanet with a stratosphere.

    Evans, Thomas M / Sing, David K / Kataria, Tiffany / Goyal, Jayesh / Nikolov, Nikolay / Wakeford, Hannah R / Deming, Drake / Marley, Mark S / Amundsen, David S / Ballester, Gilda E / Barstow, Joanna K / Ben-Jaffel, Lotfi / Bourrier, Vincent / Buchhave, Lars A / Cohen, Ofer / Ehrenreich, David / García Muñoz, Antonio / Henry, Gregory W / Knutson, Heather /
    Lavvas, Panayotis / Etangs, Alain Lecavelier des / Lewis, Nikole K / López-Morales, Mercedes / Mandell, Avi M / Sanz-Forcada, Jorge / Tremblin, Pascal / Lupu, Roxana

    Nature

    2017  Band 548, Heft 7665, Seite(n) 58–61

    Abstract: Infrared radiation emitted from a planet contains information about the chemical composition and vertical temperature profile of its atmosphere. If upper layers are cooler than lower layers, molecular gases will produce absorption features in the ... ...

    Abstract Infrared radiation emitted from a planet contains information about the chemical composition and vertical temperature profile of its atmosphere. If upper layers are cooler than lower layers, molecular gases will produce absorption features in the planetary thermal spectrum. Conversely, if there is a stratosphere-where temperature increases with altitude-these molecular features will be observed in emission. It has been suggested that stratospheres could form in highly irradiated exoplanets, but the extent to which this occurs is unresolved both theoretically and observationally. A previous claim for the presence of a stratosphere remains open to question, owing to the challenges posed by the highly variable host star and the low spectral resolution of the measurements. Here we report a near-infrared thermal spectrum for the ultrahot gas giant WASP-121b, which has an equilibrium temperature of approximately 2,500 kelvin. Water is resolved in emission, providing a detection of an exoplanet stratosphere at 5σ confidence. These observations imply that a substantial fraction of incident stellar radiation is retained at high altitudes in the atmosphere, possibly by absorbing chemical species such as gaseous vanadium oxide and titanium oxide.
    Sprache Englisch
    Erscheinungsdatum 2017--02
    Erscheinungsland England
    Dokumenttyp Journal Article ; Research Support, Non-U.S. Gov't ; Research Support, U.S. Gov't, Non-P.H.S.
    ZDB-ID 120714-3
    ISSN 1476-4687 ; 0028-0836
    ISSN (online) 1476-4687
    ISSN 0028-0836
    DOI 10.1038/nature23266
    Datenquelle MEDical Literature Analysis and Retrieval System OnLINE

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