Apsidal motion and fundamental parameters of eclipsing binary systems provide a test of stellar interiors and stellar evolution models. We completed a photometric and spectroscopic analysis of one such system, BW Aquarii. We modeled the K2 C3 light curve using ELC to determine several orbital and stellar parameters, then measured the eclipse times to determine updated apsidal motion parameters for the system. Furthermore, we obtained high resolution spectra of BW Aqr using the CHIRON echelle spectrograph on the CTIO 1.5m for radial velocity analysis. We then disentangled the spectra of each component using Doppler tomography and compared the individual spectra to BLUERED models to determine the atmospheric parameters of each component. Finally, we compared the combined photometric and spectroscopic results to the predictions of several stellar evolution models.
K2 C0 Eclipsing Binary near EPIC 202062176
We completed a photometric and light curve analysis of an eccentric eclipsing
binary in the K2 Campaign 0 feld that resides in Sh 2-252E, a
young star cluster embedded in an H II region. Because there dozens of stars in this embedded
cluster fall within the Kepler aperture, we obtained spectra of the three brightest stars in the
crowded aperture to identify which is the binary system. We found that none of these stars are
components of the eclipsing binary system, which must
be one of the fainter nearby stars. However, these bright cluster members
all have remarkable spectra: Sh 2-252a (EPIC 202062176) is a B0.5 V star with
razor sharp absorption lines, Sh 2-252b is a Herbig A0 star with disk-like emission
lines, and Sh 2-252c is a pre-main sequence star with very red color.
Lester, K.V., Gies, D.R., & Guo, Z. 2016, AJ, 152, 194
My NASA/ADS publications can be found HERE.