Comparing the precision 2009 and 2012 light curves of the precontact W UMa binary V1001 Cassiopeia
- Faculty Research Affiliate, Pisgah Astronomical Research Institute, One Pari Drive, Rosman, NC 28772 (United States)
- Physics and Engineering Dept., 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)
A 2012 follow up to the analysis of 2009 observations is presented for the very short period (∼0.43 days) precontact W UMa binary (PCWB) V1001 Cassiopeia. Its short period, similar to the majority of W UMa binaries, and its distinct EA light curve make it a very rare and interesting system for continuing photometric investigation. Previous photometric VRI standard magnitudes give a K4 spectral type. Our solutions of light curves separated by some three years give approximately the same physical parameters. However, the spots have radically changed in temperature, area, and position. While only one dark spot was used to model the first curves, two hot spots are now needed. This affects the overall shape of the light curve, especially in the secondary eclipses in B and V. Additional eclipse timings now show that the orbital period is changing. We conclude that spots are very active on this solar-type dwarf system and that it may mimic its larger cousins, the RS CVn binaries. The conclusion is that analysis now needs to be directed at the continuous time evolution of PCWBs.
- OSTI ID:
- 22342156
- Journal Information:
- Astronomical Journal (New York, N.Y. Online), Vol. 149, 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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