Light Curves of Two Eclipsing Binary Systems, BL Eridani and GW Cephei

Details Light Curves of Two Eclipsing Binary Systems, BL Eridani and GW Cephei Light Curves of Two Eclipsing Binary Systems, BL Eridani and GW Cephei

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..240..123h&link_type=abstract

Binary Stars as Critical Tools and Tests in Contemporary Astrophysics, International Astronomical Union. Symposium no. 240, he

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present light curves of two short period binary systems, BL Eridani and GW Cephei. The BL Eridani was observed with VRI filters on 5 nights at Siding Spring Observatory (SSO) by the 50cm wide field robotic telescope equipped with a 2K CCD camera, which was developed by Korea Astronomy and Space Science Institute (KASI), and Yonsei University Observatory (YUO). Two nights were observed at SSO by automatic operation mode, and three nights were observed by automatic remote observation mode from KASI in Korea. With light curves covering full phase, five new times of minimum lights were determined. The magnitude difference of primary minimum and secondary minimum with V filter appeared as 0.25 magnitude, similar to the observation by Yamasaki (1998). The light curves were analyzed by mode 3 of WD binary code, and q-search method, which shows the best fit at q = 0.48 and i = 88.7 deg. Short period contact binary system GW Cephei was observed on 5 nights by the 61cm telescope with a 2K CCD camera at Sobaeksan Optical Astronomy Observatory (SOAO) of KASI with standard BVR filters. Full light curves were obtained, and five new times of minimum light were determined. We analyzed period variation of this system with 96 times of minimum light including our observations, which shows systematic variations that can be interpreted as the light time effect by a third body with a minimum mass of 0.17 solar mass. We assumed a cool spot on the surface of the massive secondary component responsible for the asymmetry of the light curves, and calculated photometric parameters of GW Cephei by WD code, which shows q = 2.59, and i = 85.4 deg with 16% fill-out factor.

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