## 5. DistanceWith galactic coordinates , the reddening to V592 Her is probably not very large. Using the stellar reddening data for this direction from Guarinos (1992), the estimated visual extinction is , which gives . then corresponds to a late-A spectral type. We can obtain crude estimates of the distance via statistical comparisons with other dwarf novae. With the orbital period hr estimated by Duerbeck & Mennickent (1998) from the superhump period, the correlation between , , and the outburst recurrence time (Warner 1987) suggests , which yields pc. The correlation between and suggests (for a superoutburst) (Warner 1995), which, when combined with the recent maximum brightness of 12.0, yields a distance of pc. A similar distance estimate can be obtained by using Eq. (11) of Warner (1987), which gives the visual magnitude of an optically thick disk with a mean surface brightness depending on and a size depending on and the white dwarf mass. With an assumed very blue disk with , we find , in agreement with the estimate above. It is possible that TOADs do not fit very well in the above correlations, in particular because the mass in the thermally critical pre-outburst disk may be significantly larger than in a typical dwarf nova, in which case the outburst disk could be brighter by 1-2 mag. In any case, however, the distance of V592 Her is certainly less than 1 kpc. © European Southern Observatory (ESO) 1999 Online publication: February 23, 1999 |