Abstract
White dwarfs represent the end point of stellar evolution for the majority of stars. As such, they are excellent astrophysical laboratories. They are structurally simple, with electron degenerate cores surrounded by thin surface layers of helium and/or hydrogen. The g-mode pulsations provide a window into their internal structure. The Whole Earth Telescope has been conducting a long-term survey of pulsating white dwarfs with the goal of providing an empirical map of convection parameters across the DA and DB instability strips. We present an overview of white dwarf asteroseismology, and discuss the current status of our survey.
Highlights
White dwarfs represent the end point of stellar evolution for the majority of stars
The Whole Earth Telescope (WET, [5]) is engaged in a long term survey to provide an empirical map of White dwarfs (WDs) convective parameters across the DA and DB instability strip
The basic premise is that the photospheric flux is delayed and/or attenuated relative to flux at the bottom of the convection zone (CZ) by an amount that depends on the thickness of the CZ
Summary
White dwarfs represent the end point of stellar evolution for the majority of stars. As such, they are excellent astrophysical laboratories. White dwarfs (WDs) are important targets for asteroseismology. WDs are structurally simple: an electron degenerate carbon/oxygen core surrounded by thin non-degenerate layers of hydrogen and helium.
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