Abstract
Certain modes in the hot ZZ Ceti stars (HDAVs) exhibit extreme pulsational stability; their periods have been observed to show a slow increase, which is theoretically accounted for by evolutionary cooling of the star. These modes are super-stable, more stable than atomic clocks and most pulsars; they will lose one cycle in a few billion years. We have begun a program to find 100 new HDAVs to do ensemble asteroseismology and to search for planetary companions. HDAVs with an orbiting planet should show a measurable reflex motion around the center of mass of the system, easily distinguishable from their slow evolutionary cooling.
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Mukadam, A. et al. (2003). Searching for the Most Stable Pulsating Stars. In: de Martino, D., Silvotti, R., Solheim, JE., Kalytis, R. (eds) White Dwarfs. NATO Science Series, vol 105. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0215-8_69
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DOI: https://doi.org/10.1007/978-94-010-0215-8_69
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