An interpretation of light curves of SV Camelopardalis by the inverse-problem method

Details An interpretation of light curves of SV Camelopardalis by the inverse-problem method An interpretation of light curves of SV Camelopardalis by the inverse-problem method

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26as..127..233d&link_type=abstract

Astronomy and Astrophysics Supplement, v.127, p.233-242

Astronomy and Astrophysics

Astrophysics

5

Stars: Activity, Eclipsing Binaries-Stars, Individual: Sv Cam, Methods Data Analysis

Scientific paper

The paper is devoted to the problem of the determination of the orbital and physical parameters of the active eclipsing binary SV Cam on the basis of the interpretation of photometric observations made by \cite[Patkos (1982)]{Pat82} during the period 1973-1981. The problem is solved in two stages: by obtaining a synthetic light curve in the case when the parameters of the corresponding Roche model \cite[(Djura\v sevic1992a)]{Dju92a} are given a priori (direct problem), and by determining the parameters of the model for which the best fit between the synthetic light curve and the observations is achieved (inverse problem) \cite[(Djura\v sevic1992b).]{Dju92b} A total of 18 light curves are analysed in the framework of the Roche model, involving one and two spotted regions on the primary component of the system (Sp G3 V), for the temperature contrast between the spotted area and the surrounding photosphere A_s=T_s/T_1=0.65. The basic parameters of the system and of the spotted areas are estimated. Throughout the whole set of the analysed light curves, a double spot model fits the observations satisfactorily. A single spot model yields a poorer fit, where the basic system parameters obtained by analysing the individual light curves show stronger variations about a mean value. That indicates that the single spot model cannot successfully reproduce the SV Cam light curve changes during the analysed period. According to the obtained results the spotted areas are formed at high latitudes and cover a significant part of the stellar surface. No clear cyclicity of the system's activity is noted from the analysed observations. There are some indications that spotted areas at high latitudes (above 70() o) correspond to an enhanced activity. Since the system's period is short (P=0fd 59), the presence of spotted regions at high latitudes can be explained by the dynamo mechanism for rapid rotators \cite[(Schussler & Solanski 1992).]{Sch92} During the analysed period the spotted areas tend to fall into a specially active longitude sectors at high latitudes, near stellar polar regions. Due to a selection effect it is possible that a more extensive observational material would correct this result to some extent. The light curve analysis allowed an estimation of the system parameters and of the active spotted regions.

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