Eruptive binaries

Eclipses of the hot spot are analysed using the Roche lobe geometry for the secondary component. The S-wave emitting region is assumed to be located in the stream going from the secondary component to the hot spot. From parametric solutions for the model parameters it results that: the radius of the disk is larger than the minimum radius defined by the angular momentum carried by the stream and smaller than the maximum size corresponding to the largest non-intersecting orbit in the three-body problem; the masses of the components are: M1>0.31Msub(solar) and possibly >0.51Msub(solar), and M2<0.05Msub(solar); a small fraction of the mass transfered from the secondary component to the disk is immediately accreted onto the white dwarf; the amount of mass stored in the disk between the outbursts is probably sufficient to explain the outburst as a sudden accretion event, like in the case of dwarf novae. (author)