CaltechAUTHORS
  A Caltech Library Service

Gravity Modes in ZZ Ceti Stars. I. Quasi-adiabatic Analysis of Overstability

Goldreich, Peter and Wu, Yanqin (1999) Gravity Modes in ZZ Ceti Stars. I. Quasi-adiabatic Analysis of Overstability. Astrophysical Journal, 511 (2). pp. 904-915. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20130227-082524842

[img]
Preview
PDF - Published Version
See Usage Policy.

228Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20130227-082524842

Abstract

We analyze the stability of g-modes in white dwarfs with hydrogen envelopes. All relevant physical processes take place in the outer layer of hydrogen-rich material, which consists of a radiative layer overlaid by a convective envelope. The radiative layer contributes to mode damping, because its opacity decreases upon compression and the amplitude of the Lagrangian pressure perturbation increases outward. The convective envelope is the seat of mode excitation, because it acts as an insulating blanket with respect to the perturbed flux that enters it from below. A crucial point is that the convective motions respond to the instantaneous pulsational state. Driving exceeds damping by as much as a factor of 2 provided ωτ_c≥1, where ω is the radian frequency of the mode and τ_c≈4τ_(th), with τ_(th) being the thermal time constant evaluated at the base of the convective envelope. As a white dwarf cools, its convection zone deepens, and lower frequency modes become overstable. However, the deeper convection zone impedes the passage of flux perturbations from the base of the convection zone to the photosphere. Thus the photometric variation of a mode with constant velocity amplitude decreases. These factors account for the observed trend that longer period modes are found in cooler DA variables. Overstable modes have growth rates of order γ~1/(nτ_ω), where n is the mode's radial order and τ_ω is the thermal timescale evaluated at the top of the mode's cavity. The growth time, γ^(−1), ranges from hours for the longest period observed modes (P≈20 minutes) to thousands of years for those of shortest period (P≈2 minutes). The linear growth time probably sets the timescale for variations of mode amplitude and phase. This is consistent with observations showing that longer period modes are more variable than shorter period ones. Our investigation confirms many results obtained by Brickhill in his pioneering studies of ZZ Cetis. However, it suffers from two serious shortcomings. It is based on the quasiadiabatic approximation that strictly applies only in the limit ωτ_c » 1, and it ignores damping associated with turbulent viscosity in the convection zone. We will remove these shortcomings in future papers.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/306705DOIUNSPECIFIED
http://iopscience.iop.org/0004-637X/511/2/904PublisherUNSPECIFIED
Additional Information:© 1999 American Astronomical Society. Received 1998 April 28; accepted 1998 September 3. We are indebted to Bradley for supplying us with models of DA white dwarfs. We thank an anonymous referee for constructive comments. Financial support for this research was provided by NSF grant 94-14232.
Funders:
Funding AgencyGrant Number
NSF94-14232
Subject Keywords:convection - stars : atmospheres - stars : oscillations - stars : variables : other - waves
Issue or Number:2
Record Number:CaltechAUTHORS:20130227-082524842
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130227-082524842
Official Citation:Gravity Modes in ZZ Ceti Stars. I. Quasi-adiabatic Analysis of Overstability Peter Goldreich and Yanqin Wu 1999 ApJ 511 904
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:37162
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:28 Feb 2013 15:43
Last Modified:03 Oct 2019 04:45

Repository Staff Only: item control page