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Table 5.

Mass transfer rates determined by fitting the SED of each system using a model consisting of a white dwarf plus steady-state accretion disc model.

Source Period log10 ( ± ±
(mins) (M yr−1) (M yr−1)
ES Cet 10.4 −7.61 0.46 2.5 × 10−8 1.6 × 10−8
SDSSJ1351 15.7 −8.58 1.13 2.6 × 10−9 2.4 × 10−9
SDSSJ1908 18.1 −6.18 0.27 6.6 × 10−7 3.1 × 10−7
HP Lib 18.4 −8.26 0.19 5.5 × 10−9 1.9 × 10−9
ASASSN-14cc 22.5 −8.63 0.14 2.3 × 10−9 6.5 × 10−10
ASASSN-14mv 41.0 −8.59 0.16 2.6 × 10−9 7.9 × 10−10
ASASSN-14ei 43.0 −10.14 0.13 7.2 × 10−11 1.9 × 10−11
SDSSJ1525 44.3 −10.15 0.46 7.1 × 10−11 4.6 × 10−11
SDSSJ1411 46.0 −10.44 0.17 3.6 × 10−11 1.2 × 10−11
GP Com 46.6 −10.64 0.25 2.3 × 10−11 1.0 × 10−11
Gaia14aae 49.7 −10.48 0.06 3.3 × 10−11 4.3 × 10−12
SDSSJ1208 53.0 −11.15 0.15 7.1 × 10−12 2.1 × 10−12
SDSSJ1137 59.6 −11.09 0.28 8.1 × 10−12 3.9 × 10−12
V396 Hya 65.1 −10.86 0.26 1.4 × 10−11 6.2 × 10−12
SDSSJ1319 65.6 −10.94 0.26 1.1 × 10−11 5.2 × 10−12

Notes. Apart from the eclipsing system (Gaia14aae), we fixed the mass of the white dwarf at M1 = 0.8 ± 0.1 M and cos(i) = 0.5. We varied radius of the accretion disc to achieve a good fit. The large error the mass transfer rate of SDSS J1505 is due to the large error on the distance.

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