Evidence for a brown dwarf in the TOAD V592 Herculis

Details Evidence for a brown dwarf in the TOAD V592 Herculis Evidence for a brown dwarf in the TOAD V592 Herculis

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...342l..45v&link_type=abstract

Astronomy and Astrophysics, v.342, p.L45-L48 (1999)

Astronomy and Astrophysics

Astrophysics

13

Accretion, Accretion Disks, Stars: Individual: V592 Her, Stars: Low-Mass, Brown Dwarfs, Stars: Novae, Cataclysmic Variables, X-Rays: Stars

Scientific paper

We present optical R and I photometry of V592 Her obtained one year before its 1998 outburst. We identify V592 Her with a faint blue star, showing variability in R with a standard deviation of ~ 0.07 mag. With mean quiescent magnitudes of R=21.5 and I=21.4, its outburst amplitude is ~ 10 mag, which is at the very upper end of the range observed for Tremendous-Outburst-Amplitude Dwarf novae. A main sequence secondary would imply a distance > 1500 pc, which is inconsistent with the absolute magnitudes in outburst and quiescence expected for a dwarf nova. We conclude that the secondary is a brown dwarf. The quiescent flux is almost completely from the white dwarf, which gives a white dwarf temperature of 10 000 K and a distance of ~ 700 pc. The non-detection in a ROSAT PSPC observation implies an upper limit to the X-ray luminosity of <~ 4x 10(30) erg s(-1) and to the accretion rate onto the white dwarf of <~ 10(-12) {M_sunyr}. Based on observations collected at McDonald Observatory, Texas

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