Show simple item record

dc.contributor.authorDésert, J.-M.
dc.contributor.authorCharbonneau, D.
dc.contributor.authorBallard, S.
dc.contributor.authorCarter, J.A.
dc.contributor.authorQuinn, S.N.
dc.contributor.authorFressin, F.
dc.contributor.authorLatham, D.W.
dc.contributor.authorTorres, G.
dc.contributor.authorLissauer, J.J.
dc.contributor.authorSasselov, D.D.
dc.contributor.authorDemory, B.-O.
dc.contributor.authorSeager, S.
dc.contributor.authorWinn, J.N.
dc.contributor.authorFortney, J.J.
dc.contributor.authorFabrycky, D.C.
dc.contributor.authorCochran, W.D.
dc.contributor.authorEndl, M.
dc.contributor.authorMacQueen, P.J.
dc.contributor.authorIsaacson, H.T.
dc.contributor.authorKnutson, H.A.
dc.contributor.authorMarcy, G.W.
dc.contributor.authorBuchhave, L.A.
dc.contributor.authorBryson, S.T.
dc.contributor.authorRowe, J.F.
dc.contributor.authorBorucki, W.J.
dc.contributor.authorChristiansen, J.L.
dc.contributor.authorHaas, M.R.
dc.contributor.authorKoch, D.
dc.contributor.authorBatalha, N.M.
dc.contributor.authorBrown, T.M.
dc.contributor.authorCaldwell, D.A.
dc.contributor.authorJenkins, J.M.
dc.contributor.authorMullally, F.
dc.contributor.authorTenenbaum, P.
dc.contributor.authorDeming, D.
dc.contributor.authorFord, E.B.
dc.contributor.authorGilliland, R.L.
dc.contributor.authorGillon, M.
dc.contributor.authorKinemuchi, K.
dc.contributor.authorStill, M.
dc.contributor.authorLucas, P.W.
dc.contributor.authorUddin, K.
dc.date.accessioned2011-11-30T12:01:24Z
dc.date.available2011-11-30T12:01:24Z
dc.date.issued2011-11-01
dc.identifier.citationDésert , J-M , Charbonneau , D , Ballard , S , Carter , J A , Quinn , S N , Fressin , F , Latham , D W , Torres , G , Lissauer , J J , Sasselov , D D , Demory , B-O , Seager , S , Winn , J N , Fortney , J J , Fabrycky , D C , Cochran , W D , Endl , M , MacQueen , P J , Isaacson , H T , Knutson , H A , Marcy , G W , Buchhave , L A , Bryson , S T , Rowe , J F , Borucki , W J , Christiansen , J L , Haas , M R , Koch , D , Batalha , N M , Brown , T M , Caldwell , D A , Jenkins , J M , Mullally , F , Tenenbaum , P , Deming , D , Ford , E B , Gilliland , R L , Gillon , M , Kinemuchi , K , Still , M , Lucas , P W & Uddin , K 2011 , ' The hot-Jupiter Kepler-17b : Discovery, obliquity from stroboscopic starspots, and atmospheric characterization ' , Astrophysical Journal, Supplement Series , vol. 197 , no. 1 , 14 . https://doi.org/10.1088/0067-0049/197/1/14
dc.identifier.issn0067-0049
dc.identifier.otherPURE: 465881
dc.identifier.otherPURE UUID: aaf46d2e-b7b2-42fb-8874-f55c57b2b04d
dc.identifier.otherScopus: 80655127961
dc.identifier.otherORCID: /0000-0002-8872-4462/work/62748824
dc.identifier.urihttp://hdl.handle.net/2299/7201
dc.description‘In these times, during the rise in the popularity of institutional repositories, the Society does not forbid authors from depositing their work in such repositories. However, the AAS regards the deposit of scholarly work in such repositories to be a decision of the individual scholar, as long as the individual's actions respect the diligence of the journals and their reviewers.’ Original article can be found at : http://iopscience.iop.org/ Copyright American Astronomical Society
dc.description.abstractThis paper reports the discovery and characterization of the transiting hot giant exoplanet Kepler-17b. The planet has an orbital period of 1.486 days, and radial velocity measurements from the Hobby-Eberly Telescope show a Doppler signal of 419.5 m s. From a transit-based estimate of the host star's mean density, combined with an estimate of the stellar effective temperature T = 5630 ± 100 from high-resolution spectra, we infer a stellar host mass of 1.06 ± 0.07 M and a stellar radius of 1.02 ± 0.03R . We estimate the planet mass and radius to be M = 2.45 0.11 M and R = 1.31 ± 0.02R . The host star is active, with dark spots that are frequently occulted by the planet. The continuous monitoring of the star reveals a stellar rotation period of 11.89 days, eight times the planet's orbital period; this period ratio produces stroboscopic effects on the occulted starspots. The temporal pattern of these spot-crossing events shows that the planet's orbit is prograde and the star's obliquity is smaller than 15°. We detected planetary occultations of Kepler-17b with both the Kepler and Spitzer Space Telescopes. We use these observations to constrain the eccentricity, e, and find that it is consistent with a circular orbit (e < 0.011). The brightness temperatures of the planet's infrared bandpasses are = 1880 ± 100 K and = 1770 ± 150 K. We measure the optical geometric albedo A in the Kepler bandpass and find A = 0.10 ± 0.02. The observations are best described by atmospheric models for which most of the incident energy is re-radiated away from the day side.en
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal, Supplement Series
dc.rightsOpen
dc.subjectplanetary systems
dc.subjectstars: individual (Kepler-17b, KIC 10619192, 2MASS 19533486+4748540)
dc.subjecteclipses
dc.subjecttechniques: photometry
dc.titleThe hot-Jupiter Kepler-17b : Discovery, obliquity from stroboscopic starspots, and atmospheric characterizationen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=80655127961&partnerID=8YFLogxK
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2011-11-01
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1088/0067-0049/197/1/14
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record