Table 3
System parameter and brightness values used for testing the predictions of the disc instability model.
| Name | MWD[M⊙] | M2[M⊙] | Inc [degree] | m V | Ref. |
|
|
|||||
| V3885 Sge | ~0.7 | ~0.475 | ~65 | 9.5 ± 0.2 | (1) |
| UX UMa | 0.9 ± 0.3 | 0.39 ± 0.15 | 70 ± 5 | 13 ± 0.2 | (2) |
| IX Vel | 0.8 ± 0.2 | 0.52 ± 0.10 | 57 ± 2 | 9.5 ± 0.2 | (3) |
| TT Ari | ~0.9 | ~0.2 | ~30 | 10.8 ± 0.2 | (4, 5) |
| Z Cam | 0.99 ± 0.15 | 0.71 ± 0.10 | 57 ± 11 | 11.5 ± 0.2 | (6) |
| SS Cyg [a] | 1.19 ± 0.05 | 0.7 ± 0.1 | 37–53 | 8.6 ± 0.2 | (7) |
| SS Cyg [b] | 0.81 ± 0.2 | 0.55 ± 0.13 | 45–56 | 8.6 ± 0.2 | (8) |
| AH Her | 0.95 ± 0.1 | 0.76 ± 0.08 | 46 ± 3 | 12.5 ± 0.2 | (9) |
| HL CMa | ~0.83± 0.1 | 0.45 ± 0.1 | ~45 | 11.5 ± 0.2 | (10) |
| RX And | 1.14 ± 0.33 | 0.48 ± 0.03 | 51 ± 9 | 11.8 ± 0.2 | (11) |
Notes. The visual brightness is taken from the AAVSO light curve during stand-still of Z Cam stars and at the end of long outbursts for SS Cyg. At these phases the DIM predicts steady state accretion at rates close to the critical accretion rate. For the NL we used an average brightness. For HL CMa several parameters are completely unconstrained and we therefore used a broad range of inclinations (30–70 degrees) and the average WD mass for CVs of 0.83 ± 0.1. For SS Cyg we used two different sets of parameter [a] and [b]. If no error for the masses is given, we assumed an uncertainty of 0.1 M⊙.
Reference. (1) Linnell et al. (2009); (2) Neustroev et al. (2011); (3) Linnell et al. (2007); (4) Gänsicke et al. (1999); (5) Wu et al. (2002); (6) Hartley et al. (2005a); (7) Friend et al. (1990); (8) Bitner et al. (2007); (9) Horne et al. (1986); (10) Hutchings et al. (1981); (11) Shafter (1983).
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