Identification and Follow-Up Observations of Low-Mass Eclipsing Binaries from Kepler
An outstanding problem in Astronomy for the past 15+ years has been that the radii of low-mass, (M 1.0 M&sun;), main-sequence stars in eclipsing binary systems are consistently about 15% larger than predicted by theoretical models. The main cause is hypothesized to be rapid rotation due to binary spin-up, as all but one of the currently known
Coughlin, Jeffrey et al.
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2011