TY - JOUR
T1 - Rotational equilibria by Lagrangian variational principle
T2 - Towards multidimensional stellar evolutions
AU - Yasutake, Nobutoshi
AU - Fujisawa, Kotaro
AU - Yamada, Shoichi
N1 - Funding Information:
We are grateful to K. Suzuki, T. Yamasaki, M. Okamoto and T. Maruyama for fruitful discussions. This work was partially supported by JSPS KAKENHI Grant Numbers 25105510, 24244036 and Grant-in-Aid for Scientific Research on Innovative Areas, No. 24103006.
Publisher Copyright:
© 2017 The Authors.
PY - 2016/12/21
Y1 - 2016/12/21
N2 - 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.
AB - 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.
KW - Stars: evolution
KW - Stars: protostars
KW - Stars: rotation
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U2 - 10.1093/mnras/stw2216
DO - 10.1093/mnras/stw2216
M3 - Article
AN - SCOPUS:85023207447
SN - 0035-8711
VL - 463
SP - 3705
EP - 3724
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -