TY - JOUR
T1 - Seismic constraints on rotation of Sun-like star and mass of exoplanet
AU - Gizon, Laurent
AU - Ballot, Jérome
AU - Michel, Eric
AU - Stahn, Thorsten
AU - Vauclair, Gérard
AU - Bruntt, Hans
AU - Quirion, Pierre Olivier
AU - Benomar, Othman
AU - Vauclair, Sylvie
AU - Appourchaux, Thierry
AU - Auvergne, Michel
AU - Baglin, Annie
AU - Barban, Caroline
AU - Baudin, Fréderic
AU - Bazot, Michaël
AU - Campante, Tiago
AU - Catala, Claude
AU - Chaplin, William
AU - Creevey, Orlagh
AU - Deheuvels, Sébastien
AU - Dolez, Noël
AU - Elsworth, Yvonne
AU - García, Rafael
AU - Gaulme, Patrick
AU - Mathis, Stéphane
AU - Mathur, Savita
AU - Mosser, Benoît
AU - Régulo, Clara
AU - Roxburgh, Ian
AU - Salabert, David
AU - Samadi, Réza
AU - Sato, Kumiko
AU - Verner, Graham
AU - Hanasoge, Shravan
AU - Sreenivasan, Katepalli R.
PY - 2013/8/13
Y1 - 2013/8/13
N2 - Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1:85+0:52 -0:42MJupiter, which implies that it is a planet, not a brown dwarf.
AB - Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1:85+0:52 -0:42MJupiter, which implies that it is a planet, not a brown dwarf.
KW - Extrasolar planets
KW - Stellar oscillations
KW - Stellar rotation
UR - http://www.scopus.com/inward/record.url?scp=84882394180&partnerID=8YFLogxK
U2 - 10.1073/pnas.1303291110
DO - 10.1073/pnas.1303291110
M3 - Article
C2 - 23898183
AN - SCOPUS:84882394180
SN - 0027-8424
VL - 110
SP - 13267
EP - 13271
JO - National Academy of Sciences. Proceedings
JF - National Academy of Sciences. Proceedings
IS - 33
ER -