dc.contributor.author | Bell, Taylor J. | |
dc.contributor.author | Zhang, Michael | |
dc.contributor.author | Cubillos, Patricio E. | |
dc.contributor.author | Dang, Lisa | |
dc.contributor.author | Fossati, Luca | |
dc.contributor.author | Todorov, Kamen O. | |
dc.contributor.author | Cowan, Nicolas B. | |
dc.contributor.author | Deming, Drake | |
dc.contributor.author | Zellem, Robert T. | |
dc.contributor.author | Stevenson, Kevin B. | |
dc.contributor.author | Crossfield, Ian J. M, | |
dc.contributor.author | Dobbs-Dixon, Ian | |
dc.contributor.author | Fortney, Jonathan J. | |
dc.contributor.author | Knutson, Heather A. | |
dc.contributor.author | Line, Michael R. | |
dc.date.accessioned | 2021-02-23T21:22:06Z | |
dc.date.available | 2021-02-23T21:22:06Z | |
dc.date.issued | 2019-07-25 | |
dc.identifier.citation | Taylor J Bell, Michael Zhang, Patricio E Cubillos, Lisa Dang, Luca Fossati, Kamen O Todorov, Nicolas B Cowan, Drake Deming, Robert T Zellem, Kevin B Stevenson, Ian J M Crossfield, Ian Dobbs-Dixon, Jonathan J Fortney, Heather A Knutson, Michael R Line, Mass loss from the exoplanet WASP-12b inferred from Spitzer phase curves, Monthly Notices of the Royal Astronomical Society, Volume 489, Issue 2, October 2019, Pages 1995–2013, https://doi.org/10.1093/mnras/stz2018 | en_US |
dc.identifier.uri | http://hdl.handle.net/1808/31459 | |
dc.description | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. | en_US |
dc.description.abstract | The exoplanet WASP-12b is the prototype for the emerging class of ultrahot, Jupiter-mass exoplanets. Past models have predicted – and near-ultraviolet observations have shown – that this planet is losing mass. We present an analysis of two sets of 3.6 and 4.5 μmSpitzer phase curve observations of the system which show clear evidence of infrared radiation from gas stripped from the planet, and the gas appears to be flowing directly toward or away from the host star. This accretion signature is only seen at 4.5 μm, not at 3.6 μm, which is indicative either of CO emission at the longer wavelength or blackbody emission from cool, ≲600 K gas. It is unclear why WASP-12b is the only ultrahot Jupiter to exhibit this mass-loss signature, but perhaps WASP-12b’s orbit is decaying as some have claimed, while the orbits of other exoplanets may be more stable; alternatively, the high-energy irradiation from WASP-12A may be stronger than the other host stars. We also find evidence for phase offset variability at the level of 6.4σ (46.2°) at 3.6 μm. | en_US |
dc.publisher | Royal Astronomical Society | en_US |
dc.rights | Copyright 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. | en_US |
dc.subject | Accretion | en_US |
dc.subject | Accretion discs | en_US |
dc.subject | Techniques: photometric | en_US |
dc.subject | Planets and satellites: individual (WASP-12b) | en_US |
dc.subject | Planet–star interactions | en_US |
dc.title | Mass loss from the exoplanet WASP-12b inferred from Spitzer phase curves | en_US |
dc.type | Article | en_US |
kusw.kuauthor | Crossfield, Ian J. M. | |
kusw.kudepartment | Physics and Astronomy | en_US |
dc.identifier.doi | 10.1093/mnras/stz2018 | en_US |
dc.identifier.orcid | https://orcid.org/0000-0003-4177-2149 | en_US |
kusw.oaversion | Scholarly/refereed, publisher version | en_US |
kusw.oapolicy | This item meets KU Open Access policy criteria. | en_US |
dc.rights.accessrights | openAccess | en_US |