Normal Modes of Oscillation for Rotating Stars. V. A New Numerical Method for Computing Nonradial Eigenfunctions

1998 ◽  
Vol 116 (1) ◽  
pp. 57-74 ◽  
Author(s):  
Maurice J. Clement
Keyword(s):  
Numerical Method ◽  
Normal Modes ◽  
Rotating Stars

Oscillations of Fast Rotating Stars: p-Modes in Centrifugally Flattened Polytropes

2004 ◽  
Vol 215 ◽  
pp. 414-415 ◽  
Author(s):  
F. Lignières ◽  
M. Rieutord
Keyword(s):  
Numerical Method ◽  
Centrifugal Force ◽  
Perturbation Methods ◽  
Mathematical Formalism ◽  
Rotating Stars ◽  
Oscillation Modes ◽  
Rapidly Rotating Stars ◽  
Fast Rotating

Oscillation modes of rapidly rotating stars have not yet been calculated with precision, rotational effects being generally approximated by perturbation methods. We developed a mathematical formalism and a numerical method which fully account for the deformation of the star by the centrifugal force. The method has been first tested in the case of Maclaurin spheroids and then applied to uniformly rotating polytropic stars.

Rapidly rotating relativistic stars

1992 ◽  
Vol 340 (1658) ◽  
pp. 391-422 ◽  
Keyword(s):  
Neutron Stars ◽  
Numerical Models ◽  
Normal Modes ◽  
Rotating Stars ◽  
Relativistic Stars ◽  
Small Oscillations ◽  
Perfect Fluids ◽  
Upper Limits ◽  
Viscosity Limit

Within the last decade, significant progress has been made in modelling rotating stars in general relativity and in relating observable properties to the equation of state of matter at high density. A formalism describing rotating perfect fluids is presented and numerical models of neutron stars are briefly discussed, with emphasis on upper limits on mass and rotation. The equations governing small oscillations are reviewed, and a variational principle appropriate both to eulerian and lagrangian perturbations is obtained. This extends to relativity an eulerian principle used to find non-axisymmetric stability points for perfect fluids. A related eulerian approach has been recently used to obtain normal modes of rotating newtonian stars. The review concludes with an outline of this work and of the two types of instability that can restrict the range of neutron stars. In particular, current work shows that several kinds of effective viscosity limit the possible role of a non-axisymmetric instability driven by gravitational waves.

scholarly journals Equilibrium structures of rapidly rotating stars with shellular rotation

2016 ◽  
Vol 12 (S329) ◽  
pp. 398-398
Author(s):  
Kotaro Fujisawa ◽  
Yu Yamamoto
Keyword(s):  
Numerical Method ◽  
Massive Stars ◽  
Core Collapse ◽  
Rotating Stars ◽  
Self Consistent ◽  
Equilibrium Structures ◽  
Rapidly Rotating Stars

AbstractWe have developed a new numerical method for obtaining self-consistent structures of rapidly rotating stars. We obtained self-consistent equilibrium structures of rapidly rotating massive stars with shellular rotation by using the method. These equilibrium structures might be useful for both evolution of rapidly rotating massive stars and progenitor models of core-collapse supernovae simulations.

Sign in / Sign up

Export Citation Format

Share Document