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A Correlation Between Stellar Activity and Hot Jupiter Emission Spectra

Knutson, Heather A. and Howard, Andrew W. and Isaacson, Howard (2010) A Correlation Between Stellar Activity and Hot Jupiter Emission Spectra. Astrophysical Journal, 720 (2). pp. 1569-1576. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20130129-133640941

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Abstract

We present evidence for a correlation between the observed properties of hot Jupiter emission spectra and the activity levels of the host stars measured using Ca II H & K emission lines. We find that planets with dayside emission spectra that are well-described by standard one-dimensional atmosphere models with water in absorption (HD 189733, TrES-1, TrES-3, WASP-4) orbit chromospherically active stars, while planets with emission spectra that are consistent with the presence of a strong high-altitude temperature inversion and water in emission orbit quieter stars. We estimate that active G and K stars have Lyman α fluxes that are typically a factor of 4-7 times higher than quiet stars with analogous spectral types and propose that the increased UV flux received by planets orbiting active stars destroys the compounds responsible for the formation of the observed temperature inversions. In this paper, we also derive a model-independent method for differentiating between these two atmosphere types using the secondary eclipse depths measured in the 3.6 and 4.5 μm bands on the Spitzer Space Telescope and argue that the observed correlation is independent of the inverted/non-inverted paradigm for classifying hot Jupiter atmospheres.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1088/0004-637X/720/2/1569DOIArticle
https://arxiv.org/abs/1004.2702arXivDiscussion Paper
ORCID:
AuthorORCID
Knutson, Heather A.0000-0002-0822-3095
Howard, Andrew W.0000-0001-8638-0320
Isaacson, Howard0000-0002-0531-1073
Additional Information:© 2010 American Astronomical Society. Received 2010 April 14; accepted 2010 July 21; published 2010 August. Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the University of California and the California Institute of Technology. Keck time has been granted by both NASA and the University of California. We thank Geoff Marcy and Debra Fischer for their generous assistance in obtaining the Keck/HIRES spectra and deriving the SME values used in this analysis, as well as Lucianne Walkowicz, Kevin Zahnle, Mark Marley, Jonathan Fortney, Drake Deming, Jean-Michel Desert, and Adam Burrows for providing invaluable commentary on various aspects of this project. H.A.K. is supported by a fellowship from the Miller Institute for Basic Research in Science. We thank the observers who contributed to the data reported here. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Scott Dahm, Hien Tran, and Grant Hill for support of HIRES and Greg Wirth for support of remote observing. A. W. H. gratefully acknowledges support from a Townes Post-doctoral Fellowship at the U. C. Berkeley Space Sciences Laboratory. Finally, the authors wish to extend special thanks to those of Hawai‘ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible.
Funders:
Funding AgencyGrant Number
Miller Institute for Basic Research in ScienceUNSPECIFIED
University of California, BerkeleyUNSPECIFIED
Subject Keywords:binaries: eclipsing; planetary systems; stars: activity; techniques: spectroscopic
Issue or Number:2
Record Number:CaltechAUTHORS:20130129-133640941
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130129-133640941
Official Citation:A Correlation Between Stellar Activity and Hot Jupiter Emission Spectra Heather A. Knutson et al. 2010 ApJ 720 1569
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36657
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:29 Jan 2013 22:06
Last Modified:03 Oct 2019 04:40

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