Testing new theoretical models of M dwarfs

Details Testing new theoretical models of M dwarfs Testing new theoretical models of M dwarfs

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010noao.prop..400s&link_type=abstract

NOAO Proposal ID #2010B-0400

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Scientific paper

The primary aim of the observations is the search for and analysis of stellar pulsations in M dwarfs, the dominant stellar population in our Galaxy, in order to test and improve theoretical models of low mass stellar structure and evolution. Our theoretical models of early type M dwarfs show that these stars can pulsate. Expected periods of oscillations depends on stellar parameters and focus around 30 min. To confirm our theoretical predictions we plan to observe at least 100 dwarfs of early M type (30 already done). Time series photometry obtained on each star will be analyzed by means of Fourier transform. In case of positive verification of our hypothesis, this analysis provides us with frequency and amplitudes of oscillation modes and we can put observational constraints on our models. The project will also be able to detect eclipsing binaries, extrasolar planets around these stars, and other types of variability.

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