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Pulsating White Dwarfs Pulsating white dwarf stars are a particular subclass of white dwarfs, and they are very useful tools for studying the interiors of stars. As the interior of the white dwarf varies and oscillates, the light signal from the celebrity will pulsate at various frequencies. By specifying the frequencies at which the star pulsates and utilizing these as boundary states in leading models, astronomers can determine the inner properties of white dwarfs. This summer I was involved in using data in the Whole Earth Telescope and CCD images to find out the frequencies at which two distinct white dwarf stars pulsate. Wallpaper on Pulsating White Dwarfs A white dwarf star is your last resting stage of 98 percent of all stars (Kawaler per 1). The extent of a white dwarf is similar to Earth, however, its own bulk is on precisely the same sequence as the Sun. To maintain such a dense star from collapsing, the center of the star, that is composed of oxygen and carbon, becomes more electron degenerate. Surrounding the center is a thin coating of helium and hydrogen. This outer layer comprises about.01 percent of the snowy dwarfвЂ™so bulk, and it extends roughly 30 miles beneath the surface (Kawaler B 133). Without the sparse вЂњblanketвЂќ of hydrogen and helium that the black dwarf would cool very rapidly. As the white dwarf cools, the discharge of heat is comparable to a kettle of warm water with a lid on it. As steam attempts to escape, then it results in the lid to the pot to maneuver up and down. Instead of the outer coating of the celebrity moving up and down, the outer layer will be different in luminosity due to nonradial pulsations/oscillations at the interior of the celebrity. The changes in luminosity are about the order of millimagnitudes (11 millimagnitudes equals a 1% change in brightness), but the osc...