Photometric and Spectroscopic Observations of Solar Type Eclipsing Binary, GSC 0620 1143

Details Photometric and Spectroscopic Observations of Solar Type Eclipsing Binary, GSC 0620 1143 Photometric and Spectroscopic Observations of Solar Type Eclipsing Binary, GSC 0620 1143

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21823001s&link_type=abstract

American Astronomical Society, AAS Meeting #218, #230.01; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a spectra, UBVRcIc photometric observations and a solution for the high amplitude, solar type eclipsing binary, GSC 0620 1143. A period study and a light curve solution are also presented.
Our observations were taken with the 0.81-m Lowell Reflector on 19, 20 and 21 September 2008 with time granted through the National Undergraduate Observatory (NURO). The high precision light curves were premodeled with Binary 3.0, and then solved with the 2004 version Wilson code. Our modeled light curves included 205 U and B, 207 V, 202 R and 203 I individual CCD observations taken with the 2K X 2K NASACAM. Spectra taken at DAO on 23 November 2008 revealed that the variable star has a spectral type of G6±1 V.
Four mean times of minimum light were determined, including HJDMin I = 2454731.6902(±0.0007)d, and HJDMin II =2454729.9049(±0.0004)d, 2454730.8790(±0.0002)d and 2454731.8532(±0.0002)d. Two more timings were found or determined from published data to determine the following light elements:
J.D. Hel Min I = 2454731.6906(±0.0021)d + 0.32469886(±0.00000044) • E.
Our Wilson Code analysis of GSC 0620 1143 revealed it to be a W-type contact binary (the less massive component, the hotter) with a mass ratio of 2.3. The system parameters from our model included a shallow fill-out of 0.08, a slight temperature difference of 205 K and an inclination of 80 degrees. Two minor hot spot regions (15 and 7 degree radii and 1.39, 1.18 TFACT values on the primary and secondary stars, respectively) were needed.
We wish to thank the American Astronomical Society small research grant program and the Arizona Space Grant for supporting this research.

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