Low-Amplitude Variability in Very-low-mass Sigma Orionis Cluster Members: Activity and Rotation at 3 Myr

Details Low-Amplitude Variability in Very-low-mass Sigma Orionis Cluster Members: Activity and Rotation at 3 Myr Low-Amplitude Variability in Very-low-mass Sigma Orionis Cluster Members: Activity and Rotation at 3 Myr

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21442208c&link_type=abstract

American Astronomical Society, AAS Meeting #214, #422.08; Bulletin of the American Astronomical Society, Vol. 41, p.692

Astronomy and Astrophysics

Astronomy

Scientific paper

Young star-forming regions host a wide range of optically variable sources, from accreting and flaring stars to those whose light is modulated by rotating spots. However, complete characterization of variability to low amplitudes and, in particular, identification of rotation periods down through substellar masses has yet to be achieved. In addition, it was recently proposed that an additional source of variability on hour timescales-- pulsation powered by deuterium burning-- may be at work in young brown dwarfs and very low mass stars. To assess and distinguish between these varied phenomena, we have carried out a dedicated monitoring campaign on confirmed low-mass members of the Sigma Orionis cluster. Our survey achieves sensitivity to periodic variations with photometric amplitudes down to several millimagnitudes. We present the census of variability over timescales ranging from minutes to days and provide new insights into the distribution of stellar rotation periods at young ages via the detection of variability due to cool surface spots.

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