Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aca....44...59s&link_type=abstract
Acta Astronomica, v.44, pp.59-74, (1994).
Astronomy and Astrophysics
Astronomy
21
Binaries: Eclipsing, Novae: Cataclysmic Variables, Stars: Individual: Ux Uma
Scientific paper
It is proposed to divide the light curves of UX UMa, according to their shapes, into two types: (1) The standard light curves, showing a well defined orbital hump, due to the hot spot, which occurs in the phase interval from about phi=-0.4 to about phi=0.1, its declining part being still visible after the eclipse. (2) The peculiar light curves, showing either an ill defined orbital hump of a much smaller amplitude, or even a depression in the phase interval, where the hump is normally present. Using a new approach, described in Paper I, the B and V light curves of UX UMa, observed between 1952 and 1961 by Johnson et al. (1954), Walker and Herbig (1954), and Krzeminski and Walker (1963), were analyzed. The standard mean light curves of 1953 and 1955 were successfully decomposed into their disk and spot components. From the analysis of the disk and spot eclipses the basic system parameters were then determined: M_1=(0.7 pm 0.2) Modot, M_2=(0.48+0.02) Modot, A=(1.05 pm 0.08) times 1011 cm, i=73.0 pm 1.8, R_d/A=0.34 pm 0.03, dot M=(6.6 pm 2.2) times 1017g/s, and the distance d=328 pm 12 pc. The value of K_1=150 pm 18 km/s, predicted from these parameters, is in perfect agreement with spectroscopic determinations. The standard light curves of March 1952, which were brighter by 0.14 -- 0.18 mag, were analyzed in the same way giving: dot M approx 8 times 1017 g/s and R_d/A approx 0.38. The analysis of the peculiar mean V light curves of 1958 and 1961, and UBV light curves of 1952 May 29 revealed that their peculiarities are due to absorption produced by "circumdisk" material. Consequently, the peculiar light curves cannot be used in the analysis of the disk or spot eclipses.
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