BVR{sub c}I{sub c} observations and analyses on V2421 Cygni, a precontact W UMa binary
- Astronomy Group, Physics and Engineering Department, Bob Jones University, 1700 Wade Hampton Boulevard, Greenville, SC 29614 (United States)
- University of South Carolina, Lancaster, 476 Hubbard Drive, Lancaster, SC 29720 (United States)
- Physics Department, Florida International University, 11200 SW 8th Street, Miami, FL 33199 (United States)
- Global Research Technology Corporation, Camarillo, CA 92562 (United States)
We present the first precision BVRI light curves, synthetic light curve solutions, and a period study for the high amplitude solar type binary, V2421 Cygni. The light curves have the appearance of an Algol (EA) type; however, it is made up of dwarf solar type components in a detached mode with a period of only 0.6331 days with an amplitude of about a full magnitude, i.e., it is a precontact W UMa binary. Flare-like disruptions occur in the light curves following the primary and secondary eclipses possibly due to the line-of-sight track of a gas stream. An associated stream spot and splash spot cause bright equatorial spots on the stellar surface of the primary star. The more massive star is the gainer, making this system a classic, albeit dwarf, Algol.
- OSTI ID:
- 22340053
- Journal Information:
- Astronomical Journal (New York, N.Y. Online), Vol. 147, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
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