The cyclic period changes of the close binary VV Ursae Majoris.

Details The cyclic period changes of the close binary VV Ursae Majoris. The cyclic period changes of the close binary VV Ursae Majoris.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...311..915s&link_type=abstract

Astronomy and Astrophysics, v.311, p.915-918

Astronomy and Astrophysics

Astrophysics

13

Binaries: Eclipsing, Stars: Activity, Stars: Magnetic Fields, Stars: Individual: Vv Uma

Scientific paper

An analysis of the set of the minimum timings of the Algol-type eclipsing binary VV UMa is presented. The period variations are cyclic with the cycle-length of 22years. They are consistent with the presence of the third body with the orbital period P_2_=22.28years and minimum mass of 0.4Msun_. The apsidal motion must be ruled out because VV UMa is a semi-detached system according to the previous analyses. The stellar magnetic activity (Applegate =1992ApJ...385..621A) of the cold convective secondary may be an alternative cause of the observed period changes. The cycle-length, the magnitude of the period change and other characteristics are consistent with the magnetic activity.

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