First Photometric Analysis of the Solar-Type Binary, V428 Cep (NSV 395), in the Field of NGC 188
Volume 44 number 2 (2016)
- Ronald G. Samec
- Astronomy Group, Department of Natural Sciences, Emmanuel College, 181 Springs Street, Franklin Springs, GA 30639; ronaldsamec@gmail.com
- Jeremy Clark
- Astronomy Program, Department of Physics and Engineering, Bob Jones University, 1700 Wade Hampton Boulevard, Greenville, SC 29614; clarky1123@gmail.com
- David Maloney
- Astronomy Program, Department of Physics and Engineering, Bob Jones University, 1700 Wade Hampton Boulevard, Greenville, SC 29614; david.edward.maloney@gmail.com
- Daniel B. Caton
- Dark Sky Observatory, Physics and Astronomy Department, Appalachian State University, 525 Rivers Street, Boone, NC 28608-2106; catondb@appstate.edu
- Danny R. Faulkner
- Director, Johnson Observatory, 1414 Bur Oak Court, Hebron, KY 41048
Abstract
Abstract. V428 Cep (of NSV 395) is a faint 15th magnitude binary observed in a study of the open cluster NGC 188. However, its distance from the core of the cluster might exclude its membership. Its light curve was classified as a short period EB type eclipsing binary with a period of 0.3079 d and an amplitude of ~0.7 mags in all curves. The difference in component temperatures is some T =180 K and its fill-out is a hefty 35%. A brief, 2.5 year period study yields, as expected, a constant period, which is 0.3076789 d. More monitoring is needed to determine its true orbital evolution. The inclination, 80º is not quite enough to produce total eclipses, so a q-search was performed. Our lowest residual solution gives a q=0.4. A cool spot was modeled on the primary component to take care of the light curve asymmetries. V428 Cep is a K-type W UMa contact binary.