Show simple item record

dc.contributor.authorDevor, Jonathan
dc.contributor.authorCharbonneau, David
dc.contributor.authorTorres, Guillermo
dc.contributor.authorBlake, Cullen H.
dc.contributor.authorWhite, Russel J.
dc.contributor.authorRabus, Markus
dc.contributor.authorO’Donovan, Francis T.
dc.contributor.authorMandushev, Georgi
dc.contributor.authorBakos, Gaspar Á.
dc.contributor.authorFűrész, Gábor
dc.contributor.authorSzentgyorgyi, Andrew
dc.date.accessioned2019-09-24T17:25:33Z
dc.date.issued2008
dc.identifier.citationDevor, Jonathan, David Charbonneau, Guillermo Torres, Cullen H. Blake, Russel J. White, Markus Rabus, Francis T. O’Donovan, et al. 2008. “T‐Lyr1‐17236: A Long‐Period Low‐Mass Eclipsing Binary.” The Astrophysical Journal 687 (2): 1253–63. https://doi.org/10.1086/592080.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41397440*
dc.description.abstractWe describe the discovery of a 0.68+0.52 M-circle dot eclipsing binary (EB) with an 8.4 day orbital period, found through a systematic search of 10 fields of the Trans-atlantic Exoplanet Survey (TrES). Such long-period low-mass EBs constitute critical test cases for resolving the long-standing discrepancy between the theoretical and observational mass-radius relations at the bottom of the main sequence. It has been suggested that this discrepancy may be related to strong stellar magnetic fields, which are not properly accounted for in current theoretical models. All previously well-characterized low-mass main-sequence EBs have periods of a few days or less, and their components are therefore expected to be rotating rapidly as a result of tidal synchronization, thus generating strong magnetic fields. In contrast, the binary system described here has a period that is more than 3 times longer than previously characterized low-mass main-sequence EBs, and its components rotate relatively slowly. It is therefore expected to have a weaker magnetic field and to better match the assumptions of theoretical stellar models. Our follow-up observations of this EB yield preliminary stellar properties that suggest it is indeed consistent with current models. If further observations confirm a low level of activity in this system, these determinations would provide support for the hypothesis that the mass-radius discrepancy is at least partly due to magnetic activity.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleT‐Lyr1‐17236: A Long‐Period Low‐Mass Eclipsing Binary
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorCharbonneau, David::a0e3ca75d3fb8511f2f554ed69428108::600
dc.date.available2019-09-24T17:25:33Z
dash.workflow.comments1Science Serial ID 97985
dc.identifier.doi10.1086/592080
dash.source.volume687;2
dash.source.page1253-1263


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record