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An improved limit for the rate of period change in the ZZ Ceti star G117-B15A or The Most Stable Optical Clock Known

  • S.O. Kepler (a1), D.E. Winget (a2), E.L. Robinson (a2) and R.E. Nather (a2)

Abstract

The rate of change of period with time for the g-mode pulsations in ZZ Ceti stars depends directly on the cooling timescale for a DA white dwarf, and therefore a measurement of its value can yield an evolutionary timescale for the white dwarf. We have obtained an upper limit for the rate of change of the period of the dominant pulsation in the light curve of the ZZ Ceti star G117-B15A of |dP/dt| ≤ 9.9 × 10−15 s/s at the 68% confidence level, equivalent to a timescale for period change of

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References

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An improved limit for the rate of period change in the ZZ Ceti star G117-B15A or The Most Stable Optical Clock Known

  • S.O. Kepler (a1), D.E. Winget (a2), E.L. Robinson (a2) and R.E. Nather (a2)

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