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dc.contributor.authorMcCann, John
dc.contributor.authorMurray-Clay, Ruth A.
dc.contributor.authorKratter, Kaitlin
dc.contributor.authorKrumholz, Mark R.
dc.date.accessioned2019-07-02T21:50:38Z
dc.date.available2019-07-02T21:50:38Z
dc.date.issued2019-03-01
dc.identifier.citationJohn McCann et al 2019 ApJ 873 89en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/ab05b8
dc.identifier.urihttp://hdl.handle.net/10150/633281
dc.description.abstractBathed in intense ionizing radiation, close-in gaseous planets undergo hydrodynamic atmospheric escape, which ejects the upper extent of their atmospheres into the interplanetary medium. Ultraviolet detections of escaping gas around transiting planets corroborate such a framework. Exposed to the stellar environment, the outflow is shaped by its interaction with the stellar wind and by the planet's orbit. We model these effects using Athena to perform 3D radiative-hydrodynamic simulations of tidally locked hydrogen atmospheres receiving large amounts of ionizing extreme-ultraviolet flux in various stellar environments for the low-magnetic-field case. Through a step-by-step exploration of orbital and stellar wind effects on the planetary outflow, we find three structurally distinct stellar wind regimes: weak, intermediate, and strong. We perform synthetic Ly alpha observations and find unique observational signatures for each regime. A weak stellar wind-which cannot confine the planetary outflow, leading to a torus of material around the star-has a pretransit, redshifted dayside arm and a slightly redward-skewed spectrum during transit. The intermediate regime truncates the dayside outflow at large distances from the planet and causes periodic disruptions of the outflow, producing observational signatures that mimic a double transit. The first of these dips is blueshifted and precedes the optical transit. Finally, strong stellar winds completely confine the outflow into a cometary tail and accelerate the outflow outward, producing large blueshifted signals posttransit. Across all three regimes, large signals occur far outside of transit, offering motivation to continue ultraviolet observations outside of direct transit.en_US
dc.description.sponsorshipNational Science Foundation [AST-1411536, -1228509]; Australian Research Council [FT180100375]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/873/i=1/a=89?key=crossref.c763dd4043160f63caeb261362bf3f1den_US
dc.rights© 2019. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjecthydrodynamicsen_US
dc.subjectmethods: numericalen_US
dc.subjectplanet-star interactionsen_US
dc.subjectplanets and satellites: atmospheresen_US
dc.subjectplanets and satellites: gaseous planetsen_US
dc.subjectradiative transferen_US
dc.titleMorphology of Hydrodynamic Winds: A Study of Planetary Winds in Stellar Environmentsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.contributor.departmentUniv Arizona, Steward Observen_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.volume873
dc.source.issue1
dc.source.beginpage89
refterms.dateFOA2019-07-02T21:50:38Z


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