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dc.contributor.authorLothringer, Joshua D.
dc.contributor.authorBarman, Travis
dc.contributor.authorKoskinen, Tommi
dc.date.accessioned2019-02-20T21:49:48Z
dc.date.available2019-02-20T21:49:48Z
dc.date.issued2018-10-10
dc.identifier.citationJoshua D. Lothringer et al 2018 ApJ 866 27en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aadd9e
dc.identifier.urihttp://hdl.handle.net/10150/631727
dc.description.abstractExtremely irradiated hot Jupiters, exoplanets reaching dayside temperatures >2000 K, stretch our understanding of planetary atmospheres and the models we use to interpret observations. While these objects are planets in every other sense, their atmospheres reach temperatures at low pressures comparable only to stellar atmospheres. In order to understand our a priori theoretical expectations for the nature of these objects, we self-consistently model a number of extreme hot Jupiter scenarios with the PHOENIX model atmosphere code. PHOENIX is well-tested on objects from cool brown dwarfs to expanding supernovae shells, and its expansive opacity database from the UV to far-IR make PHOENIX well-suited to understanding extremely irradiated hot Jupiters. We find several fundamental differences between hot Jupiters at temperatures >2500 K and their cooler counterparts. First, absorption by atomic metals like Fe and Mg, molecules including SiO and metal hydrides, and continuous opacity sources like H-, all combined with the short-wavelength output of early-type host stars, result in strong thermal inversions, without the need for TiO or VO. Second, many molecular species, including H2O, TiO, and VO are thermally dissociated at pressures probed by transit and eclipse observations, potentially biasing retrieval algorithms that assume uniform vertical abundances. We discuss other interesting properties of these objects, as well as future prospects and predictions for observing and characterizing this unique class of astrophysical object, including the first self-consistent model of the hottest known Jovian planet, KELT-9b.en_US
dc.description.sponsorshipNASA through the Space Telescope Science Institute [HST-GO-12511, HST-GO-14797]; NASA [NAS 5-26555]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/866/i=1/a=27?key=crossref.310d83e7805cdc7e06c28610a89ed591en_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.subjectmethods: numericalen_US
dc.subjectplanets and satellites: atmospheresen_US
dc.titleExtremely Irradiated Hot Jupiters: Non-oxide Inversions, H- Opacity, and Thermal Dissociation of Moleculesen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume866
dc.source.issue1
dc.source.beginpage27
refterms.dateFOA2019-02-20T21:49:49Z


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