Long-term photometric behaviour of the RS CVn binary RT Lacertae

Details Long-term photometric behaviour of the RS CVn binary RT Lacertae Long-term photometric behaviour of the RS CVn binary RT Lacertae

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...405..733c&link_type=abstract

Astronomy and Astrophysics, v.405, p.733-745 (2003)

Astronomy and Astrophysics

Astrophysics

8

Stars: Activity, Binaries: Close, Stars: Individual: Rt Lacertae, Starspots

Scientific paper

A sequence of the seasonal light curves of RT Lac, covering the period 1978-2000, is analysed in the framework of the starspot hypothesis to define the spot distribution, based on the interpretation of the B-band observations. The analysis of the corresponding light curves is made using Djurašević's inverse-problem method. To explain the light-curve variations we modelled the binary system using a Roche model that involved regions containing spots on both components. Satisfactory fits were obtained assuming spots on both components. The more-massive G5 primary appears to be the most active star in the system and its spotted areas are mainly responsible for the light-curve distortions. Spots are concentrated around longitudes 45degr -170degr and at high latitudes (above 45degr ). Our analysis indicates two spots with diameters of ~ 10degr -50degr on both hemispheres of the primary. However, the less-massive cool component seems to have only one spot which covers a relatively small area. Total spotted area of the more-massive primary component indicates clear evidence for a short-term activity cycle with a period of 8.4 yr, and a possible long-term cycle with a period of 33.5 yr. The G9IV secondary does not show any evidence for an activity cycle, its spot coverage appearing rather constant at about 10% of its surface. The variation of the orbital period seems to be correlated with the total activity level of the system. In particular, the decrement of the orbital period appears to be associated with minimum spottedness and sizeable changes of the surface spot pattern distribution on the surface of each star. This result, if confirmed by the future observations, can provide further support for recently proposed models for connection between the magnetic activity and orbital period variations.

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