Table 5
System properties.
| Source | MWD | Ṁ | D ∗ |
| M⊙ | M⊙ yr-1 | pc | |
|
|
|||
| IGR J0839 | 0.95 ± 0.08 | 3.2 × 10-10 | 1200 |
| IGR J1830 | 0.85 ± 0.06 | 2.4 × 10-11 | 100 |
| IGR J1650 | 0.92 ± 0.06 | 4.1 × 10-11 | 270 |
| IGR J1817 | 0.96 ± 0.05 | 2.4 × 10-10 | 610 |
| IGR J1719 | 0.86 ± 0.06 | 1.9 × 10-11 | 130 |
| V2069 Cyg | 0.82 ± 0.08 | 5.3 × 10-10 | 930 |
| RX J0636 | 0.74 ± 0.06 | 5.4 × 10-10 | 1100 |
| IRG J1509 | 0.89 ± 0.08 | 2.5 × 10-10 | 600 |
| XSS J0056 | 0.79 ± 0.07 | 2.5 × 10-10 | 320 |
Notes. WD masses as derived from maximum post-shock temperature (Col. 2). Lower limits to the mass accretion rate (Col. 3) adopting the source distances (reported in Col. 4) and the orbital periods (in the last column of Table 2).
Lower limits to the distances are determined as follows: we used the lower uncertainty values of the adopted orbital periods and the 2MASS K band (reddening correction not applied) magnitudes of the optical counterparts. For the secondary stars we used the K band absolute magnitudes predicted for CV donors as a function of Porb (Knigge 2006), assuming that these donors totally contribute to the K band flux.
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