Photometric Solution of the Eclipsing Binary V351 Pegasi

Details Photometric Solution of the Eclipsing Binary V351 Pegasi Photometric Solution of the Eclipsing Binary V351 Pegasi

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ap%26ss.296..293a&link_type=abstract

Astrophysics and Space Science, Volume 296, Issue 1-4, pp. 293-296

Astronomy and Astrophysics

Astrophysics

Binaries, Close-Binaries, Eclipsing-V351 Peg

Scientific paper

BVR light curves of the recently discovered eclipsing binary V351 Peg were studied to derive the preliminary physical parameters of the system. The light curves were obtained at the TÜBİTAK* Turkish National Observatory (TUG) during three nights in August, 2003. The solutions were made using Djurašević’s inverse problem method. V351 Peg is a system in an overcontact configuration (f over˜ 21 %) with a relatively small temperature difference between the components ΔT ≈ 20 K. The results suggest a significant mass and energy transfer from the more massive primary onto the less massive secondary. The hot area on the less massive star, near the neck region, can be considered as a consequence of this mass and energy exchange between the components through the connecting neck of the common envelope.

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