Stellar Variability

Sinusoidal Stellar Variability Catalog

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Non-Synchronized Rotation in Close Eclipsing Binary

There is a well-known discrepancy between observations and theoretical models for K and M stars, in that they are observed to be larger and cooler than predicted. This discrepancy could be attributed to enhanced magnetic fields and starspot activity that block convection and, thus, causes an inflation in the stellar radius. In Fetherolf et al. (2019), we measured the properties of the KIC 8736245 eclipsing binary system using ground-based photometry from Mount Laguna Observatory and the 4-year Kepler light curve. KIC 8736245 is a circular eclipsing binary system that consists of a G-type star leaving the Main Sequence and a K-type star that are each spinning super- and sub-synchronously compared to the 5.07 day orbital period (see periodogram on the left). Overall, this system proves to be an interesting case study for the exchange of angular momentum as binary stars evolve off the Main Sequence.

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