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New Photometric Observations of RS Oph

Published online by Cambridge University Press:  17 January 2013

Irina Voloshina  and
Vladimir Metlov
Irina Voloshina
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij prospect 13, Moscow 119992, Russia email: vib@sai.msu.ru
Vladimir Metlov
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij prospect 13, Moscow 119992, Russia email: vib@sai.msu.ru
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Abstract

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The recurrent nova RS Oph is a long period (~455 days) binary system consisting of a hot white dwarf with mass close to the Chandrasekhar limit and an M-type giant secondary. Here we present the results of photometric observations of this nova which were made during recent years with the telescopes of the Sternberg Astronomical Institute in Crimea.

Keywords

stars: novaecataclysmic variablesoscillationsindividual (RS Oph)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 201 - 202
Copyright
Copyright © International Astronomical Union 2013

References

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Voloshina, I. & Metlov, V. 2009, in: Soonthornthum, B., Komonjinda, S., Cheng, K. S., & Leung, K. C. (eds.), The Eight Pacific Rim Conference on Stellar Astrophisics, Proc. of the conference held 5-9 May, 2008, Phuket, Thailand (San Francisco: ASP), 404 p. 72Google Scholar