All Tables

Table 1: M₂ for P_h = 1.829 and P_h = 3.439 from various M₂-P relations or different $\alpha$ and $\beta$ values in the literature (see text).
Table 2: The system inclination for M₁ = 1.25-1.40 $M_{\odot }$ and K₁ = 24 $\pm$ 5 km s^-1 for the cases (1) P_h = 1 $.\!\!^{\rm h}$ 829, M₂ = 0.12; and (2) P_h = 3 $.\!\!^{\rm h}$ 439, M₂ = 0.24.
Table 3: M₁, R₁, the factor $\phi$ = (R₁/M₁)/(R_1o/M_1o), the post-1967 mass accretion rate $\dot{M}$ (for $L_{\rm disk}$ = 70 $L_{\odot }$ ), the ignition mass, and the recurrence time $\tau$ = $M_{\rm ign}$ / $\dot{M}$ (see Sect. 8).
Table 4: The basic quantities.
Table 5: M₁, the estimated pre-1967-outburst accretion rate $\dot{M}_{\rm pre-OB}$ (for $L_{\rm disk}$ = 140 $L_{\odot }$ ), the theoretical ignition mass $M_{\rm ign}$ , the accreted mass $M_{\rm accr}$ = 22 $\cdot$ $\dot{M}_{\rm pre-OB}$ and the expected recurrence time $\tau$ = $M_{\rm ign}$ / $\dot{M}_{\rm pre-OB}$ .
Table 6: A comparison between Yaron et al. (2005) grids and observations.
Table 7: XMM observations compared with IUE fluxes and ground based photometry.