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dc.contributor.authorHussain, Gaitee Ara Jaffer
dc.contributor.authorAlvarado-Gómez, J. D.
dc.contributor.authorGrunhut, J.
dc.contributor.authorDonati, J.-F.
dc.contributor.authorAlecian, E.
dc.contributor.authorOksala, M.
dc.contributor.authorMorin, J.
dc.contributor.authorFares, Rim
dc.contributor.authorJardine, Moira Mary
dc.contributor.authorDrake, J. J.
dc.contributor.authorCohen, O.
dc.contributor.authorMatt, S.
dc.contributor.authorPetit, P.
dc.contributor.authorRedfield, S.
dc.contributor.authorWalter, F. M.
dc.date.accessioned2016-02-24T13:10:09Z
dc.date.available2016-02-24T13:10:09Z
dc.date.issued2016-01
dc.identifier.citationHussain , G A J , Alvarado-Gómez , J D , Grunhut , J , Donati , J-F , Alecian , E , Oksala , M , Morin , J , Fares , R , Jardine , M M , Drake , J J , Cohen , O , Matt , S , Petit , P , Redfield , S & Walter , F M 2016 , ' A spectro-polarimetric study of the planet-hosting G dwarf, HD 147513 ' , Astronomy & Astrophysics , vol. 585 , A77 . https://doi.org/10.1051/0004-6361/201526595en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 241204903
dc.identifier.otherPURE UUID: 92828380-b1d0-4146-aeb8-44ee84b72088
dc.identifier.otherBibCode: 2016A&A...585A..77H
dc.identifier.otherScopus: 84952683013
dc.identifier.otherWOS: 000369710300084
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821863
dc.identifier.urihttp://hdl.handle.net/10023/8299
dc.description.abstractThe results from a spectro-polarimetric study of the planet-hosting Sun-like star, HD 147513 (G5V), are presented here. Robust detections of Zeeman signatures at all observed epochs indicate a surface magnetic field, with longitudinal magnetic field strengths varying between 1.0–3.2 G. Radial velocity variations from night to night modulate on a similar timescale to the longitudinal magnetic field measurements. These variations are therefore likely due to the rotational modulation of stellar active regions rather than the much longer timescale of the planetary orbit (Porb = 528 d). Both the longitudinal magnetic field measurements and radial velocity variations are consistent with a rotation period of 10 ± 2 days, which are also consistent with the measured chromospheric activity level of the star (′log R′HK = -4.64). Together, these quantities indicate a low inclination angle, i ~ 18°. We present preliminary magnetic field maps of the star based on the above period and find a simple poloidal large-scale field. Chemical analyses of the star have revealed that it is likely to have undergone a barium-enrichment phase in its evolution because of a higher mass companion. Despite this, our study reveals that the star has a fairly typical activity level for its rotation period and spectral type. Future studies will enable us to explore the long-term evolution of the field, as well as to measure the stellar rotation period, with greater accuracy.
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2015. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1051/0004-6361/201526595en
dc.subjectStars: activityen
dc.subjectStars: magnetic fielden
dc.subjectStars: solar-typeen
dc.subjectStars: individual: HD 147513en
dc.subjectTechniques: polarimetricen
dc.subjectTechniques: radial velocities, stars: individual: WASP-1, stars: individual: WASP-24, stars: individual: WASP-38, stars: individual: HAT-P-8, planetary systemsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleA spectro-polarimetric study of the planet-hosting G dwarf, HD 147513en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201526595
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016A%26A...585A..77Hen


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