On the Nature of Continuum and Hα Emission Variations of V471 Tau-type Stars

Details On the Nature of Continuum and Hα Emission Variations of V471 Tau-type Stars On the Nature of Continuum and Hα Emission Variations of V471 Tau-type Stars

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21915343b&link_type=abstract

American Astronomical Society, AAS Meeting #219, #153.43

Mathematics

Scientific paper

Two close binaries composed of a white dwarf and a red dwarf, V471 Tau and DE CVn, were photometrically monitored with narrowband filters using the CCD-equipped 24-inch and 17-inch telescopes of the Maria Mitchell Observatory. This allowed us to separate the variability of Hα emission from that of the continuum. V471 Tau demonstrated variations in both continuum and line emission similar to what was known from its previous spectroscopy - a double-humped light curve in continuum, with maxima at phases 0.25 and 0.75, and a single-peaked curve in emission, with a maximum at phase 0.5. However, DE CVn showed a double peaked light curve in both the continuum and line emission, which indicates that the line emission is distributed over the surface of the red dwarf similarly to the continuum, not just concentrated in the area illuminated by the white dwarf. Evidence was found for occasional cycle to cycle variations of at least ±5% in both stars. At least one event of emission line flare of approximately 20% was registered in DE CVn, followed by a drop of continuum flux by approximately 15%, on a time scale of 1 day. A possible interpretation involves chromospheric flares in the red companion followed by the development of large dark spots. This project was supported by NSF/REU grant AST-0851892, the Presidential Award for Excellence in Science, Mathematics and Engineering Mentoring and the Nantucket Maria Mitchell Association.

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