Measuring Stellar Oscillations Using Spitzer: P-Modes in the Hyades

Details Measuring Stellar Oscillations Using Spitzer: P-Modes in the Hyades Measuring Stellar Oscillations Using Spitzer: P-Modes in the Hyades

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20772b&link_type=abstract

Spitzer Proposal ID #20772

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Scientific paper

Observations of oscillations in solar-like stars are limited by the fact that the level of variability involved is typically very small (approximately 4-5 parts per million at optical wavelengths). While heroic efforts have made it possible to detect oscillations in a few solar-like stars from the ground, the most astrophysically interesting targets -- those in nearby open clusters -- are unreachable and likely to remain so for many years. Solar observations have shown that the amplitude of oscillations seen in the 4.7-micron CO lines is nearly two orders of magnitude higher than that seen at optical wavelengths. For solar-like stars, such lines dominate the spectrum in IRAC Band 2. In fact, we estimate that the amplitude of p-mode oscillations in that band will be approximately 200 parts per million. This is 40 times the level in the optical, and easily accessible using Spizer. We propose a long time series of observations of the star VB 64, in the Hyades. We anticipate being able to detect a number of distinct oscillation modes, and thus to determine the large separation. In combination with other, previously measured, physical parameters of VB 64, we expect to be able to determine values for mass, age, and chemical composition which are at least an order of magnitude more precise that has been previously possible for any star in the Hyades.

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