2016/09/04 by Nobutoshi Yasutake, Kotaro Fujisawa, Shoichi Yamada · 5 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Baroclinity #Barotropic fluid #Classical mechanics #Field (mathematics) #Geometry #Lagrangian #Mechanics #Physics #Rotation (mathematics) #Rotational symmetry #Solar and Space Plasma Dynamics #Stars #Stellar, planetary, and galactic studies #Theoretical physics #Variational principle #astro-ph.EP #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stw2216
published in Monthly Notices of the Royal Astronomical Society 463(4), 3705-3724 (Oxford University Press) · 23 pages, 28 figures, accepted for publishing in MNRAS
arxiv created 2016/09/04 · openalex publication_date 2016/09/05 · openalex created_date 2016/09/16 · arxiv updated 2016/09/21 · openalex updated_date 2026/08/05
We have developed a new formulation to obtain self-gravitating, axisymmetric configurations in permanent rotation. The formulation is based on the Lagrangian variational principle with a triangulated mesh. It treats not only barotropic but also baroclinic equations of state. We compare the various stellar equilibria obtained by our new scheme with those by Hachisu's self-consistent field scheme for the barotropic case, and those by Fujisawa's self-consistent field scheme for the baroclinic case. Included in these rotational configurations are those with shellular-type rotations, which are commonly assumed in the evolution calculation of rotating stars. Although radiation processes, convections and meridional flows have not been taken into account in this study, we have in mind the application of this method to the two-dimensional evolution calculations of rotating stars, for which the Lagrangian formulation is best suited.