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A spectro-polarimetric study of the planet-hosting G dwarf, HD 147513

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Date
01/2016
Author
Hussain, Gaitee Ara Jaffer
Alvarado-Gómez, J. D.
Grunhut, J.
Donati, J.-F.
Alecian, E.
Oksala, M.
Morin, J.
Fares, Rim
Jardine, Moira Mary
Drake, J. J.
Cohen, O.
Matt, S.
Petit, P.
Redfield, S.
Walter, F. M.
Funder
Science & Technology Facilities Council
Science & Technology Facilities Council
Grant ID
ST/M001296/1
ST/J001651/1
Keywords
Stars: activity
Stars: magnetic field
Stars: solar-type
Stars: individual: HD 147513
Techniques: polarimetric
Techniques: radial velocities, stars: individual: WASP-1, stars: individual: WASP-24, stars: individual: WASP-38, stars: individual: HAT-P-8, planetary systems
QB Astronomy
QC Physics
NDAS
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Abstract
The 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.
Citation
Hussain , 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/10.1051/0004-6361/201526595
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201526595
ISSN
0004-6361
Type
Journal article
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/10.1051/0004-6361/201526595
Collections
  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2016A%26A...585A..77H
URI
http://hdl.handle.net/10023/8299

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