The rate of period change in pulsating DB white dwarf stars

@article{Crsico2004TheRO,
  title={The rate of period change in pulsating DB white dwarf stars},
  author={Alejandro H. C{\'o}rsico and Leandro G. Althaus},
  journal={Astronomy and Astrophysics},
  year={2004},
  volume={428},
  pages={159-170}
}
In this work, we present the theoretically expected rates of pulsation period change for V777 Her (DBV) vari- able stars. To this end we employ new evolutionary models representative of pulsating DB white dwarf stars computed in a self-consistent way with the predictions of time-dependent element diffusion. At the hot edge of the DB instability strip, the envelopes of the models are characterized by a diffusion-induced double-layered chemical structure. We compute the numerical values of rates… Expand
View PDF on arXiv
11 Citations
Background Citations
4
Methods Citations
2

11 Citations

Citation Type

Citation Type

Peculiar variations of white dwarf pulsation frequencies and maestro
In Part I we report on variations of the normal mode frequencies of the pulsating DB white dwarfs EC 20058-5234 and KIC 8626021 and the pulsating DA white dwarf GD 66. The observations of EC… Expand
Asteroseismology of the Kepler Field DBV White Dwarf. It is a Hot One
We present an asteroseismic analysis of the helium atmosphere white dwarf (a DBV) recently found in the field of view of the Kepler satellite. We analyze the five-mode pulsation spectrum that was… Expand
The pulsations of PG 1351+489
PG 1351+489 is one of the 20 DBVs ― pulsating helium-atmosphere white dwarf stars ― known and has the simplest power spectrum for this class of star, making it a good candidate to study cooling… Expand
Axions and the white dwarf luminosity function
The evolution of white dwarfs can be described as a simple cooling process. Recently, it has been possible to determine with an unprecedented precision their luminosity function, that is, the number… Expand
First axion bounds from a pulsating helium-rich white dwarf star
The Peccei-Quinn mechanism proposed to solve the CP problem of Quantum Chromodynamics has as consequence the existence of axions, hypothetical weakly interacting particles whose mass is constrained… Expand
Seven-Period Asteroseismic Fit of the Kepler DBV
We present a new, better-constrained asteroseismic analysis of the helium-atmosphere (DB) white dwarf discovered in the field of view of the original Kepler mission. Observations obtained over the… Expand
Pulsating low-mass white dwarfs in the frame of new evolutionary sequences - IV. The secular rate of period change
We present a theoretical assessment of the expected temporal rates of change of periods ($\dot{\Pi}$) for low-mass ($M_{\star}/M_{\sun} \lesssim 0.45$) and extremely low-mass (ELM,… Expand
Analysis of IUE spectra of helium-rich white dwarf stars
We studied the class of DB white dwarf stars, using re-calibrated UV spectra for thirty four DBs obtained with the IUE satellite. By comparing the observed energy distributions with model… Expand
Axions and the cooling of white dwarf stars
W hite dwarfsare the end productofthe lifes ofinterm ediate-and low-m assstarsand their evolution is described as a sim ple cooling process. Recently,it has been possible to determ ine with an… Expand
An Observer's View on the Future of Asteroseismology
Scientific research is a continuous process, and the speed of future progress can be estimated by the pace of finding explanations for previous research questions. In this observer’s based view of… Expand
...
1
2
...

References

SHOWING 1-10 OF 44 REFERENCES
New DA white dwarf evolutionary models and their pulsational properties
In this letter we investigate the pulsational properties of ZZ Ceti stars on the basis of new white dwarf evolutionary models calculated in a self-consistent way with the predictions of time… Expand
Evolutionary period changes in rotating hot pre-white dwarf stars
We have calculated and splitting of high order nonradial g-modes due to slow rotation in models of hot pre-white dwarf (''PWD'') stars of 0.60 M/sub sun/. We have investigated the effects of… Expand
Theoretical Models for Asteroseismology of DA White Dwarf Stars
Because white dwarfs are the most common end state of stellar evolution, determining their internal structure will yield many clues about the final stages of stellar evolution and the physics of… Expand
New evolutionary models for massive ZZ Ceti stars. I. First results for their pulsational properties
We present new and improved evolutionary calculations for carbon-oxygen white dwarf (WD) stars appropriate for the study of massive ZZ Ceti stars. To this end, we follow the complete evolution of… Expand
The potential for asteroseismology of DB white dwarf stars
We present the results of a parametric survey of evolutionary models of compositionally stratified white dwarfs with helium surface layers (DB white dwarfs). Because white dwarfs are the most common… Expand
Asteroseismology of white dwarf stars. I - Adiabatic results
A preliminary investigation of the asteroseismological properties of chemically stratified evolutionary DA and DB white dwarf models is reported. The period and kinetic energy distributions for… Expand
Evolutionary models for pulsation studies of white dwarfs
A large grid of equilibrium models suitable for adiabatic and nonadiabatic seismological investigations of pulsating white dwarfs of the DAV and DBV types is presented and discussed in detail. The… Expand
Constraining the Evolution of ZZ Ceti
We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. On the basis of observations that span 31 years, we… Expand
A detection of the evolutionary time scale of the DA white dwarf G117 - B15A with the Whole Earth Telescope
The time rate of change for the main pulsation period of the 13,000 K DA white dwarf G117 - B15A has been detected using the Whole Earth Telescope (WET). The observed rate of period change, P(dot) =… Expand
A Strong Test of Electro-Weak Theory using Pulsating DB White Dwarf Stars as Plasmon Neutrino Detectors
We demonstrate that plasmon neutrinos are the dominant form of energy loss in model white dwarf stars down to T_eff ~ 25,000 K, depending on the stellar mass. The lower end of this range overlaps the… Expand
...
1
2
3
4
5
...