Open AccessRotation speed and stellar axis inclination from p modes: how CoRoT would see other suns
Author(s) -
Ballot J.,
García R. A.,
Lambert P.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.10375.x
Subject(s) - physics , rotation (mathematics) , suns in alchemy , context (archaeology) , astrophysics , solar rotation , rotation period , stars , monte carlo method , dispersion (optics) , stellar rotation , astronomy , optics , solar physics , geometry , paleontology , statistics , mathematics , biology
In the context of future space‐based asteroseismic missions, we have studied the problem of extracting the rotation speed and the rotation‐axis inclination of solar‐like stars from the expected data. We have focused on slow rotators (at most twice solar rotation speed), first, because they constitute the most difficult case and, secondly, because some of the Convection Rotation and planetary Transits ( CoRoT ) main targets are expected to have slow rotation rates. Our study of the likelihood function has shown a correlation between the estimates of inclination of the rotation axis i and the rotational splitting δν of the star. By using the parameters, i and δν ⋆ =δν sin i , we propose and discuss new fitting strategies. Monte Carlo simulations have shown that we can extract a mean splitting and the rotation‐axis inclination down to solar rotation rates. However, at the solar rotation rate we are not able to correctly recover the angle i , although we are still able to measure a correct δν ⋆ with a dispersion less than 40 nHz.