Star-planet interactions. I. Stellar rotation and planetary orbits
Informazioni aggiuntive
Autori
Privitera G.,
Meynet G.,
Eggenberger P.,
Vidotto A. a.
Tipo
Articolo pubblicato in rivista scientifica
Anno
2016
Lingua
Inglese
Abstract
Context. As a star evolves, planet orbits change over time owing totidal interactions, stellar mass losses, friction and gravitational drag forces, mass accretion, and evaporation on/by the planet. Stellar rotation modifies the structure of the star and therefore the way these different processes occur. Changes in orbits, subsequently, have an impact on the rotation of the star.
Aims: Models that account in a consistent way for these interactions between the orbital evolution of the planet and the evolution of the rotation of the star are still missing. The present work is a first attempt to fill this gap.
Methods: We compute the evolution of stellar models including a comprehensive treatment of rotational effects, together with the evolution of planetary orbits, so that the exchanges of angular momentum between the star and the planetary orbit are treated in a self-consistent way. The evolution of the rotation of the star accounts for the angular momentum exchange with the planet and also follows the effects of the internal transport of angular momentum and chemicals. These rotating models are computed for initial masses of the host star between 1.5 and 2.5 M$_⊙$, with initial surface angula
Aims: Models that account in a consistent way for these interactions between the orbital evolution of the planet and the evolution of the rotation of the star are still missing. The present work is a first attempt to fill this gap.
Methods: We compute the evolution of stellar models including a comprehensive treatment of rotational effects, together with the evolution of planetary orbits, so that the exchanges of angular momentum between the star and the planetary orbit are treated in a self-consistent way. The evolution of the rotation of the star accounts for the angular momentum exchange with the planet and also follows the effects of the internal transport of angular momentum and chemicals. These rotating models are computed for initial masses of the host star between 1.5 and 2.5 M$_⊙$, with initial surface angula
Rivista
Astronomy and Astrophysics
Volume
591
Pagina inizio
A45
Parole chiave
irsol-refereed-scientific-papers
