Structure of Uniformly Rotating Stars
arXiv:1105.0588 · doi:10.1088/0004-637X/735/2/69
Abstract
Zero age main sequence models of uniformly rotating stars have been computed for ten masses between 1.625 and 8 M_\odot and 21 rotation rates from zero to nearly critical rotation. The surface shape is used to distinguish rotation rather than the surface equatorial velocity or the rotation rate. Using the surface shape is close to, but not quite equivalent to using the ratio of the rotation rate to the critical rotation rate. Using constant shape as the rotation variable means that it and the mass are separable, something that is not true for either the rotation rate or surface equatorial velocity. Thus a number of properties, including the ratio of the effective temperature anywhere on the surface to the equatorial temperature, are nearly independent of the mass of the model, as long as the rotation rate changes in such a way to keep the surface shape constant.
ApJ accepted
References in corpus (10)
- Imaging the Surface of Altair
- Effects of gravitational darkening on the determination of fundamental parameters in fast rotating B-type stars
- Acoustic oscillations of rapidly rotating polytropic stars. II. Effects of the Coriolis and centrifugal accelerations
- Acoustic oscillations in rapidly rotating polytropic stars I. Effects of the centrifugal distortion
- Imaging and Modeling Rapidly Rotating Stars: Alpha Cephei and Alpha Ophiuchi
- Regular patterns in the acoustic spectrum of rapidly rotating stars
- On the Structure and Properties of Differentially Rotating Main-Sequence Stars in the 1-2 M_sun Range
- Radial and Nonradial Oscillation Modes in Rapidly Rotating Stars
- Rotationally-modulated g-modes in the rapidly-rotating delta Scuti star Rasalhague (alpha Ophiuchi)
- Rotational Splitting of Pulsational Modes
Cited by in corpus (11)
- Interferometric Observations of Rapidly Rotating Stars
- The Transit Light Source Effect II: The Impact of Stellar Heterogeneity on Transmission Spectra of Planets Orbiting Broadly Sun-like Stars
- An algorithm for computing the 2D structure of fast rotating stars
- Analysis of Spin-Orbit Misalignment in Eclipsing Binary DI Herculis
- Theoretical p Mode Oscillation Frequencies for the Rapidly Rotating Delta Scuti Star Alpha Ophiuchi
- Ab initio modelling of steady rotating stars
- Matching the Spectral Energy Distribution and p Mode Oscillation Frequencies of the Rapidly Rotating Delta Scuti Star ? Ophiuchi with a 2D Rotating Stellar Model
- Convection in Oblate Solar-Type Stars
- Modeling rotating stars in two dimensions
- Scaling of Observable Properties in Rapidly Rotating Stars
- Scaling of oscillation frequencies in rotating stars