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Eclipsing binaries are important tools for studying stellar evolution andstellar interiors. Their accurate fundamental parameters are used to testevolutionary models, and systems showing apsidal motion can also be used totest the model's internal structure predictions. For this purpose, we present aphotometric and spectroscopic analysis of the eclipsing binary BW Aquarii, anevolved F-type binary with slow apsidal motion. We model the K2 C3 light curveusing the Eclipsing Light Curve code to determine several orbital and stellarparameters, as well as measure the eclipse times to determine updated apsidalmotion parameters for the system. Furthermore, we obtain high-resolutionspectra of BW Aqr using the CHIRON echelle spectrograph on the CTIO 1.5m forradial velocity analysis. We then reconstruct the spectra of each componentusing Doppler tomography in order to determine the atmospheric parameters. Wefind that both components of BW Aqr are late F-type stars with M1 = 1.365 +/-0.008 Msun, M2 = 1.483 +/- 0.009 Msun, and R1 = 1.782 +/- 0.021 Rsun, R2 =2.053 +/- 0.020 Rsun. We then compare these results to the predictions ofseveral stellar evolution models, finding that the models cannot reproduce theobserved properties of both components at the same age.

A Photometric, Spectroscopic, and Apsidal Motion Analysis of the F-type Eclipsing Binary BW Aquarii from K2 Campaign 3