CCD Observations and the First Analysis of the Totally Eclipsing, Extreme-Mass-Ratio Binary, GSC 06462-00195

Volume 52 number 1 (2024)

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Ronald G. Samec

Pisgah Astronomical Research Institute, 112 Idlewood Acres, Hartwell, GA 30643; ronaldsamec@gmail.com

Daniel Caton

Dark Sky Observatory, Department of Physics and Astronomy, Appalachian State University, 525 Rivers Street, Boone, NC 28608-2106; catondb@appstate.edu

Danny R. Faulkner

Johnson Observatory, 1414 Bur Oak Court, Hebron, KY 41048; dfaulkner@answersingenesis.org

Walter van Hamme

Department of Physics, Florida International University, Miami, FL 33199; Southeastern Association for Research in Astronomy (SARA) Observatory; vanhamme@fiu.edu

Abstract

GSC 06462-00195 is an eclipsing binary with a mean V magnitude of 11.52, an amplitude of V~ 0.28 magnitude, a period of 0.6334857 d, and a color index of J–K = 0.211 mag. The ASAS-SN light curve suggests the variable as an extreme-mass-ratio, total eclipsing, W UMa-type binary. Six BVRI eclipse timings were observed with the CTIO reflector, and eight times of low light were taken from ASAS-SN observations. From our present observations, we determined the linear period of 0.63348292 d. Presently, the period appears to be increasing over the 22.2-year period study. A Wilson-Devinney analysis reveals that the system is an A-type (more massive component is the hottest) W UMa-type binary with an extreme mass ratio, q = 0.0937 ± 0.0001. Its fill-out is 66 ± 2%. One hot spot was needed to model a slight light curve asymmetry. The temperature difference of the components is ~ 416 K. The inclination of ~ 82.5° results in a long time of totality in the primary eclipse, with a duration of ~ 109.5 minutes, or 1.82 hours.