2. Primary minima:
3. MinII = 15m.92.
4. The infrared colors J–H = 0.666, H–K = 0.152 and J–K = 0.818
are consistent with the
dK spectral type (Bessell and Brett 1988) and BY: classification.
5. ELL type is also possible. Variability with P1 = 0d.2969
is probably caused
by non-spherical shapes of the stars; variability with P2 = 0d.2980
by a spotted photosphere region of one of the close binary's components.
P1 differing from P2 means that, in this case, we can deal
whose components are not in corotation.
MinII = 14m.87.
6. MinII = 13m.14.
7. O'Connell effect. Primary minima:
During observations of the field of the cataclysmic variable V496 Aur, we discovered
seven new variable stars.
Our observations were carried out at the Astrotel-Caucasus observatory using the
Ritchey–Chretien telescope, equipped with an unfiltered Apogee Alta U9000 CCD
A total of 664 images with 5-minute exposures were obtained on JD 2455503 –
For basic reductions for dark current, flat fields, bias, and for removing cosmic-ray
hits, we used IRAF routines.
For search and photometry of new variable stars, we applied VaST software by Sokolovsky
Lebedev (2005). The comparison star was USNO-A2.0 1275-06936213 = USNO-B1.0 1304-0181013
(α = 07h28m26s.86, δ = +40°25′
R1 = 13m.87, R2 = 14m.50
(USNO-B1.0). Unfiltered magnitudes were calibrated using the comparison star, assuming
Rcomp = 14m.185.
The coordinates of the variable stars in the Table were drawn from the 2MASS catalogue
(Skrutskie et al. 2006).
For search for periods and epochs of extrema, we use Peranso
Bessell, M.S., Brett, J.M., 1988, PASP, 100, 1134
Skrutskie, M.F., Cutri, R.M., Stiening, R., et al., 2006, AJ, 131, 1163
Sokolovsky, K., Lebedev, A., 2005, in 12th Young Scientists' Conference on Astronomy
and Space Physics, Kyiv, Ukraine, April 19–23, 2005, eds.: Simon, A.; Golovin, A.,