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Hα Variability in PTFO8-8695 and the Possible Direct Detection of Emission from a 2 Million Year Old Evaporating Hot Jupiter

Johns-Krull, Christopher M. and Prato, Lisa and McLane, Jacob N. and Ciardi, David R. and van Eyken, Julian C. and Chen, Wei and Stauffer, John R. and Beichman, Charles A. and Frazier, Sarah A. and Boden, Andrew F. and Morales-Calderón, María and Rebull, Luisa M. (2016) Hα Variability in PTFO8-8695 and the Possible Direct Detection of Emission from a 2 Million Year Old Evaporating Hot Jupiter. Astrophysical Journal, 830 (1). Art. No. 15. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20161005-072304972

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Abstract

We use high time cadence, high spectral resolution optical observations to detect excess Hα emission from the 2–3 Myr old weak-lined T Tauri star PTFO 8-8695. This excess emission appears to move in velocity as expected if it were produced by the suspected planetary companion to this young star. The excess emission is not always present, but when it is, the predicted velocity motion is often observed. We have considered the possibility that the observed excess emission is produced by stellar activity (flares), accretion from a disk, or a planetary companion; we find the planetary companion to be the most likely explanation. If this is the case, the strength of the Hα line indicates that the emission comes from an extended volume around the planet, likely fed by mass loss from the planet which is expected to be overflowing its Roche lobe.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/0004-637X/830/1/15DOIArticle
http://iopscience.iop.org/article/10.3847/0004-637X/830/1/15PublisherArticle
https://arxiv.org/abs/1606.02701arXivDiscussion Paper
ORCID:
AuthorORCID
Ciardi, David R.0000-0002-5741-3047
Stauffer, John R.0000-0003-3595-7382
Rebull, Luisa M.0000-0001-6381-515X
Additional Information:© 2016 American Astronomical Society. Received 2015 September 14; revised 2016 May 11; accepted 2016 May 19; published 2016 October 3. L.P. and C.M.J.-K. wish to acknowledge partial support for this research from the NASA Origins of Solar Systems program through grant number 07-SSO07-86 made to Lowell Observatory. CMJ-K also wishes to acknowledge partial support for this work from the National Science Foundation through grant number 1212122 made to Rice University. This work was funded in part through the 2013–2014 NAU/NASA Space Grant Undergraduate Research Internship for Jacob N. McLane. Finally, we wish to thank an anonymous referee for several useful comments that improved the original manuscript.
Group:Palomar Transient Factory, Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA07-SSO07-86
NSFAST-1212122
Northern Arizona UniversityUNSPECIFIED
NASA Space Grant Undergraduate Research InternshipUNSPECIFIED
Subject Keywords:accretion, accretion disks; line: profiles; stars: atmospheres; stars: formation; stars: magnetic field; stars: pre-main sequence
Issue or Number:1
Record Number:CaltechAUTHORS:20161005-072304972
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161005-072304972
Official Citation:Christopher M. Johns-Krull et al 2016 ApJ 830 15
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:70848
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:05 Oct 2016 14:56
Last Modified:03 Oct 2019 16:01

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