Prospects for Asteroseismology of Rapidly Rotating B-Type Stars

  title={Prospects for Asteroseismology of Rapidly Rotating B-Type Stars},
  author={Hideyuki Saio},
  journal={arXiv: Solar and Stellar Astrophysics},
  • H. Saio
  • Published 2 February 2013
  • Physics
  • arXiv: Solar and Stellar Astrophysics
In rapidly rotating stars, Coriolis forces and centrifugal deformations modify the properties of oscillations; the Coriolis force is important for low-frequency modes, while the centrifugal deformation affects mainly p-modes. Here, we discuss properties of g- and r-mode oscillations in rotating stars. Predicted frequency spectra of high-order g-modes (and r-modes) excited in rapidly rotating stars show frequency groupings associated with azimuthal order m. We compare such properties with… 
Rapidly rotating B stars with viscous Keplerian decretion disks
In the past decade, a consensus has emerged regarding the nature of clas- sical Be stars: They are very rapidly rotating main sequence B stars, which, through a still unknown, but increasingly
Equation of state effects on gravitational waves from rotating core collapse
Gravitational waves (GWs) generated by axisymmetric rotating collapse, bounce, and early postbounce phases of a galactic core-collapse supernova are detectable by current-generation gravitational
Frequency Analysis of a Potential SPB Star η Tau
: In this study, five years of photometric data of η Tau obtained from the STEREO satellite between 2007 and 2011 are presented. The high-precision data are compared with the results derived from the
Photometric investigations of several early-type variable stars using the stereo satellite
We present results from high-precision photometric monitoring of several bright early-type stars. The data cover five years and are collected by the STEREO satellite. Stellar types covered are a
In this study, high-precision photometric data of V960 Tau are presented in order to reveal the pulsation characteristics of the star. The data are taken from the HI-1A instrument of the STEREO
Classifying Be Star Variability With TESS. I. The Southern Ecliptic
TESS photometry is analyzed for 430 classical Be stars observed in the first year of the mission. The often complex and diverse variability of each object in this sample is classified to obtain an


R-mode oscillations in uniformly rotating stars
R-mode (or quasi-toroidal mode) oscillations in uniformly and slowly rotating stars have been investigated. Perturbations of the gravitational potential have been included. Applying an adiabatic
On non-radial oscillations of B-type stars.
The excitation mechanisms behind the slow pulsations―with periods of the order of one day―of OB stars are discussed on the basis of numerical computations. Non-radial, non-adiabatic stability
Kappa‐mechanism excitation of retrograde mixed modes in rotating B‐type stars
I examine the stability of retrograde mixed modes in rotating B-type stars. These modes can be regarded as a hybrid between the Rossby modes that arise from conservation of vorticity, and the
Pulsational Stability of g-Modes in Slowly Pulsating B Stars
Low-frequency g-modes excited by the opacity bump mechanism in main-sequence stars with the masses M ~ 4 M☉ are believed to be responsible for the periodic variability observed in slowly pulsating B
Stability of g modes in rotating B-type stars
We have studied the stability of low-degree g modes in uniformly rotating B-type stars, taking into account the effects of the Coriolis force and the rotational deformation. From an analysis treating
Observational Asteroseismology of slowly pulsating B stars
We review the status of observational asteroseismology of slowly pulsating B (SPB) stars. Their asteroseismic potential is extremely good because the excited high-order g-modes probe the deep
Unstable quasi g-modes in rotating main-sequence stars
This paper studies the oscillatory stability of uniformly rotating main-sequence stars of mass 3−8 Mby solving the linearized non-adiabatic, non-radial oscillation equations with a forcing term and
Fundamental parameters of Be stars located in the seismology fields of COROT
In preparation for the COROT space mission, we determined the fundamental parameters (spectral type, temperature, gravity, vsini) of the Be stars observable by COROT in its seismology fields (64 Be
Low-Frequency Oscillations in Rotating Stars
We review the properties of low-frequency oscillations in uniformly rotating stars. Rotation not only yields a new class of modes, like inertial modes and r-modes, but also significantly modifies the