Other
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...8e..33s&link_type=abstract
Solar and Stellar Activity Cycles, 26th meeting of the IAU, Joint Discussion 8, 17-18 August 2006, Prague, Czech Republic, JD08,
Other
Scientific paper
We present new CCD observations of XZ CMi. A UBVRI light curve analysis and an updated periodicity study are given. Our study shows that the orbital period is decreasing and there is a low amplitude 23-year oscillation in the O-C diagram. Both of these phenomena could be associated with the presence of stellar magnetic activity. XZ CMi is found to be a short-period Algol-type near-contact binary. Our CCD observations were taken 08-12 March 2005 with the Lowell 31-inch reflector and a liquid nitrogen cooled CCD camera with a metachrome coated TEK 512 X 512 chip. Standard UBVR--[c]I[c] filters were used. Some 127 times of minimum light have been determined^2-50. The data show a parabolic trend as well as a low amplitude (0.0051 days, or a light-time of 0.9 AU) oscillation in the quadratic residuals: HJD Tmin I = 24 53441.77225 ± 0.00125 + 0.57880796 ± 0. 00000010*E - 3.5 X 10^ -11 ± 0.3 × 10^-11 d*E^2 + (0.0051 ± 0.0007) Sin[(4.28 × 10^-4 ± 0.1 × 10^-4)*E + 6.2 ± 0.2] We note that 23-year sinusoidal oscillation would be expected from solar-type magnetic cycles. We suggest that high energy observations from spacecraft be undertaken to verify this. A simultaneous BVRI Wilson code solution was obtained revealing that the system is an Algol-type with the secondary, less massive component filling its Roche-lobe and the primary under filling. The third light values varied from 17-18%. The fill-out of the primary component was 92%. Other results are outlined on the poster.
We suggest that precision timings afforded by today's CCD detectors should be analyzed for the effect of magnetic cycles as was done here.
Faulkner Danny R.
Samec Ronald G.
van Hamme Walter
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