The DOI matches its Crossref record; 150 of the 150 references it cites were found in a registry or an index.
COMPOSITIONAL DIVERSITY IN THE ATMOSPHERES OF HOT NEPTUNES, WITH APPLICATION TO GJ 436b
Open accessAbstract
Neptune-sized extrasolar planets that orbit relatively close to their host stars—often called "hot Neptunes"—are common within the known population of exoplanets and planetary candidates. Similar to our own Uranus and Neptune, inefficient accretion of nebular gas is expected produce hot Neptunes whose masses are dominated by elements heavier than hydrogen and helium. At high atmospheric metallicities of 10–10,000 times solar, hot Neptunes will exhibit an interesting continuum of atmospheric compositions, ranging from more Neptune-like, H 2 -dominated atmospheres to more Venus-like, CO 2 -dominated atmospheres. We explore the predicted equilibrium and disequilibrium chemistry of generic hot Neptunes and find that the atmospheric composition varies strongly as a function of temperature and bulk atmospheric properties such as metallicity and the C/O ratio. Relatively exotic H 2 O, CO, CO 2 , and even O 2 -dominated atmospheres are possible for hot Neptunes. We apply our models to the case of GJ 436b, where we find that a CO-rich, CH 4 -poor atmosphere can be a natural consequence of a very high atmospheric metallicity. From comparisons of our results with Spitzer eclipse data for GJ 436b, we conclude that although the spectral fit from the high-metallicity forward models is not quite as good as the best fit obtained from pure retrieval methods, the atmospheric composition predicted by these forward models is more physically and chemically plausible in terms of the relative abundance of major constituents. High-metallicity atmospheres (orders of magnitude in excess of solar) should therefore be considered as a possibility for GJ 436b and other hot Neptunes.
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Cites
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Cited by
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“…observations are made, our knowledge of these worlds comes from our limited observations and from various models that have been validated against the rocky planets, ice giants, and gas giants we have in our solar system (e.g., Line et al., 2011; Moses et al., 2013; Miguel and Kaltenegger, 2014).”
Metadata
- Authors
- Moses, J. I., Line, M. R., Visscher, C., Richardson, M. R., Nettelmann, N., Fortney, J. J., Barman, T. S., Stevenson, K. B., & Madhusudhan, N.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2013-10-11
- Volume
- 777
- Issue
- 1
- Pages
- 34
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2127232021
- Cited by
- 299
- References
- 150
- FWCI
- 9.66
- Type
- journal article
- Language
- en
- Open access
- bronze
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- Moses, J. I., Line, M. R., Visscher, C., Richardson, M. R., Nettelmann, N., Fortney, J. J., Barman, T. S., Stevenson, K. B., & Madhusudhan, N. (2013). COMPOSITIONAL DIVERSITY IN THE ATMOSPHERES OF HOT NEPTUNES, WITH APPLICATION TO GJ 436b. The Astrophysical Journal. https://doi.org/10.1088/0004-637x/777/1/34
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