Enhanced mass transfer during dwarf nova outbursts by irradiation of the secondary?

Free access article

Issue		A&A Volume 428, Number 2, December III 2004


Page(s)		L17 - L20
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:200400093

A&A 428, L17-L20 (2004)
DOI: 10.1051/0004-6361:200400093

Letter

Enhanced mass transfer during dwarf nova outbursts by irradiation of the secondary?

Y. Osaki¹ and F. Meyer²

¹ Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
e-mail: osaki@astron.s.u-tokyo.ac.jp
² Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85740 Garching, Germany

(Received 9 August 2004 / Accepted 9 October 2004)

Abstract
One of the remaining issues in the problems of dwarf novae is whether or not enhanced mass transfer due to irradiation of the secondary stars could occur during outbursts. In a previous paper (Osaki & Meyer 2003), we presented a theoretical analysis that shows no appreciable enhancement of the mass outflow rate. This conclusion is challenged by Smak (2004) who claims that equations used in our analysis were incorrect and that in systems with short orbital periods substantial enhancement could occur. In this letter, we examine the origin of such divergent conclusions. We show that Smak's solutions are unacceptable from the standpoint of the equation of continuity and that our analysis is an appropriate one to treat this problem.

Key words: accretion, accretion disks -- binaries: close -- novae, cataclysmic variables -- stars: dwarf novae

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