Pulsating White Dwarfs

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Pulsating White Dwarfs

Pulsating white dwarf stars are a special subclass of white dwarfs, and they are very useful tools for studying the interiors of stars. As the interior of the white dwarf changes and oscillates, the light signal from the star will pulsate at numerous frequencies. By determining the frequencies at which the star pulsates and using these as boundary conditions in stellar models, astronomers can determine the interior properties of white dwarfs. This summer I was involved in using data from the Whole Earth Telescope and CCD images to determine the frequencies at which two different white dwarf stars pulsate.

Background on Pulsating White Dwarfs

A white dwarf star is the final resting stage of 98 % of all stars (Kawaler A 1). The size of a white dwarf is comparable to Earth, but its mass is on the same order as the Sun. To keep such a dense star from collapsing, the core of the star, which is composed of carbon and oxygen, becomes electron degenerate. Surrounding the core is a thin layer of helium and hydrogen. This outer layer contains about .01% of the white dwarf’s mass, and it extends about 30 miles below the surface (Kawaler B 133). Without the thin “blanket” of hydrogen and helium, the white dwarf would cool very rapidly.

As the white dwarf cools, the release of heat is comparable to a pot of boiling water with a lid on it. As steam tries to escape, it causes the lid on the pot to move up and down. Instead of the outer layer of the star moving up and down, the outer layer will vary in luminosity due to nonradial pulsations/oscillations in the interior of the star. The changes in luminosity are on the order of millimagnitudes (11 millimagnitudes equals a 1% change in brightness), but the osc...

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... this summer were to perform data reduction on light curves of pulsating white dwarfs and to gain research experience. Over the course of the summer, I was successful in reducing the data of a pulsating white dwarf taken with WET because I

had found the independent frequencies at which the star pulsates. Besides being successful in find the independent frequencies, I also gained experience doing data reduction of light curves taken by WET and also CCD images. In the future, my experience may even allow me to take part of the next WET run.

Works Cited

Kawaler, Steven D. and Winget, Donald E. “White Dwarfs: Fossil Stars.” Sky and Telescope. August 1987.

Kawaler, Steven D. and Dahlstrom, Michael. “White Dwarf Stars.” American Scientist. In press 2000.

Nather, Edward R. and Winget, Donald E. “Taking the Pulse of White Dwarfs.” Sky and Telescope. April 1992.

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