Table 4.
Main results of this study.
| (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | |
|---|---|---|---|---|---|---|---|---|---|---|
| Object | EB − V | PL index | VAAVSO | VPL + AV |
 |
 |
 |
 |
log ṀW | log ṀP |
| [mag] | [mag] | [mag] | [mag] | [mag] | [L⊙] | [L⊙] | [M⊙ yr−1] | [M⊙ yr−1] | ||
| PX And | 0.0 | *−0.15±0.06 | 15.0±0.8 | 14.3±0.1 | 5.1±0.8 | 4.7±0.9 | 1.1±0.3 | 1.7±0.6 | −9.00±0.16 | −8.81±0.18 |
| V794 Aql | 0.12±0.06 | −1.94±0.04 | 14.5±0.5 | 14.2±0.2 | 5.5±0.6 | 5.6±0.7 | 2.0±0.5 | 1.8±0.7 | −8.74±0.16 | −8.79±0.21 |
| V1315 Aql | 0.30±0.10 | −0.61±0.08 | 14.2±0.3 | 13.9±0.3 | 3.6±0.7 | 3.1±0.8 | 3.5±1.8 | 7.2±4.6 | −8.49±0.24 | −8.18±0.29 |
| HL Aqr | 0.10±0.03 | −2.16±0.01 | 13.3±0.2 | 13.4±0.1 | 4.9±0.2 | 5.1±0.2 | 3.0±0.2 | 2.4±0.2 | −8.55±0.12 | −8.66±0.11 |
| UU Aqr | 0.14±0.04 | −1.03±0.05 | 13.0±0.5 | 12.9±0.2 | 4.5±0.6 | 4.1±0.7 | 1.7±0.6 | 3.2±1.4 | −8.79±0.18 | −8.54±0.22 |
| TT Ari | 0.04±0.02 | −1.92±0.01 | 10.6±0.5 | 10.4±0.1 | 4.2±0.5 | 4.3±0.5 | 5.8±0.4 | 4.7±0.5 | −8.27±0.12 | −8.37±0.11 |
| WX Ari | 0.08±0.03 | −0.73±0.06 | 15.0±0.4 | 14.9±0.1 | 5.8±0.6 | 5.6±0.7 | 0.5±0.2 | 0.6±0.3 | −9.38±0.19 | −9.27±0.26 |
| KR Aur | 0.08±0.04 | −1.56±0.02 | 13.3±0.6 | 13.1±0.1 | 5.4±0.7 | 5.5±0.7 | 1.5±0.4 | 1.3±0.4 | −8.86±0.15 | −8.93±0.16 |
| V363 Aur | 0.27±0.05 | −1.93±0.01 | 14.4±0.4 | 14.3±0.2 | 3.5±0.6 | 3.1±0.7 | 10.8±3.8 | 16.7±8.8 | −8.00±0.19 | −7.82±0.25 |
| BZ Cam | 0.05±0.03 | −1.40±0.01 | 12.6±0.6 | 12.4±0.1 | 5.2±0.6 | 5.4±0.6 | 1.5±0.2 | 1.2±0.2 | −8.87±0.12 | −8.96±0.14 |
| QU Car | 0.11±0.04 | −2.36±0.01 | 11.4±0.4 | 11.5±0.1 | 2.2±0.4 | 2.1±0.5 | 41.0±5.1 | 50.2±10.0 | −7.42±0.12 | −7.34±0.14 |
| V425 Cas | 0.15±0.05 | −1.38±0.05 | 15.0±1.0 | 15.0±0.2 | 5.3±1.0 | 5.5±1.0 | 1.1±0.1 | 0.9±0.1 | −9.00±0.12 | −9.09±0.12 |
| V592 Cas | 0.19±0.06 | −2.22±0.01 | 12.4±0.2 | 12.5±0.2 | 4.1±0.3 | 4.2±0.3 | 6.8±0.6 | 5.7±0.9 | −8.20±0.12 | −8.29±0.12 |
| AC Cnc | 0.09±0.03 | −0.60±0.03 | 14.1±0.2 | 14.3±0.1 | 4.1±0.3 | 3.8±0.4 | 1.5±0.4 | 2.4±0.8 | −8.87±0.16 | −8.67±0.18 |
| V751 Cyg | 0.23±0.10 | −0.74±0.02 | 13.8±0.4 | 13.2±0.3 | 4.3±0.6 | 4.4±0.6 | 2.8±0.6 | 2.4±0.8 | −8.58±0.14 | −8.66±0.18 |
| CM Del | 0.14±0.05 | −1.97±0.01 | 13.7±0.4 | 13.5±0.2 | 5.4±0.7 | 5.2±0.9 | 2.2±1.0 | 2.6±1.9 | −8.69±0.24 | −8.63±0.35 |
| RZ Gru | 0.02±0.02 | −1.69±0.01 | 12.3±0.4 | 12.4±0.1 | 3.5±0.5 | 3.3±0.5 | 7.3±1.6 | 9.0±3.1 | −8.17±0.15 | −8.09±0.18 |
| V795 Her | 0.02±0.02 | −1.70±0.01 | 12.5±0.5 | 12.2±0.1 | 4.1±0.6 | 4.2±0.6 | 5.5±1.2 | 5.1±1.9 | −8.29±0.15 | −8.33±0.19 |
| V825 Her | 0.0 | −1.97±0.02 | 13.6±0.8 | 14.4±0.0 | 4.1±0.8 | 4.3±0.8 | 2.7±0.2 | 2.1±0.2 | −8.61±0.12 | −8.72±0.11 |
| BH Lyn | 0.08±0.02 | *−0.25±0.09 | 15.4±1.0 | 15.1±0.1 | 4.7±1.1 | 4.2±1.1 | 1.0±0.4 | 1.9±0.9 | −9.01±0.20 | −8.76±0.24 |
| BP Lyn | 0.0 | −1.80±0.01 | 14.3±0.2 | 14.0±0.0 | 5.6±0.5 | 5.7±0.8 | 1.5±0.6 | 1.4±1.0 | −8.87±0.22 | −8.91±0.34 |
| MV Lyr | 0.0 | −1.17±0.02 | 12.5±0.5 | 13.0±0.0 | 4.8±0.5 | 5.0±0.5 | 0.9±0.0 | 0.7±0.0 | −9.07±0.11 | −9.18±0.11 |
| AH Men | 0.08±0.02 | −1.71±0.01 | 12.7±0.3 | 12.9±0.1 | 4.2±0.4 | 4.2±0.4 | 2.6±0.5 | 2.7±0.9 | −8.61±0.14 | −8.60±0.18 |
| HQ Mon | 0.06±0.03 | −2.10±0.01 | 12.9±0.5 | 13.1±0.1 | 4.0±0.6 | 4.1±0.6 | 6.1±1.1 | 5.3±1.7 | −8.25±0.14 | −8.31±0.17 |
| KQ Mon | 0.04±0.02 | −1.67±0.01 | 13.1±0.3 | 12.6±0.1 | 4.5±0.5 | 4.5±0.7 | 4.9±1.8 | 4.5±2.8 | −8.35±0.20 | −8.39±0.29 |
| V380 Oph | 0.12±0.04 | −1.00±0.05 | 14.3±0.4 | 13.9±0.2 | 5.1±0.5 | 5.2±0.5 | 1.3±0.3 | 1.2±0.4 | −8.92±0.15 | −8.96±0.18 |
| V426 Oph | 0.14±0.04 | −1.98±0.01 | 12.5±0.8 | 11.5±0.1 | 5.8±0.8 | 5.7±0.9 | 3.2±0.7 | 3.6±1.3 | −8.53±0.15 | −8.48±0.18 |
| V442 Oph | 0.18±0.08 | −1.94±0.01 | 13.8±0.4 | 13.6±0.2 | 5.0±0.7 | 4.9±0.9 | 2.8±1.4 | 3.2±2.6 | −8.58±0.24 | −8.54±0.37 |
| LQ Peg | 0.0 | −1.80±0.03 | 14.8±0.3 | 14.8±0.1 | 5.0±0.3 | 5.1±0.3 | 2.2±0.3 | 1.7±0.3 | −8.69±0.12 | −8.80±0.13 |
| LS Peg | 0.09±0.03 | −1.73±0.01 | 11.7±0.4 | 11.6±0.1 | 4.7±0.4 | 4.8±0.4 | 2.8±0.2 | 2.4±0.3 | −8.58±0.12 | −8.66±0.12 |
| TW Pic | 0.01±0.01 | −0.94±0.02 | 13.8±0.2 | 12.8±0.0 | 6.2±0.2 | 6.3±0.2 | 0.9±0.1 | 0.7±0.1 | −9.10±0.12 | −9.17±0.12 |
| V347 Pup | 0.05±0.03 | −0.68±0.03 | 13.5±0.5 | 13.3±0.1 | 4.3±0.9 | 3.7±1.0 | 2.0±1.4 | 4.4±3.7 | −8.74±0.32 | −8.40±0.38 |
| V348 Pup | 0.0 | *−0.61±0.04 | 15.6±0.2 | 15.4±0.1 | 4.8±0.5 | 4.3±0.6 | 1.1±0.5 | 2.2±1.2 | −9.00±0.22 | −8.71±0.27 |
| VY Scl | 0.0 | −1.87±0.01 | 12.8±0.6 | 12.4±0.0 | 4.5±0.6 | 4.6±0.7 | 5.3±0.8 | 4.5±1.2 | −8.31±0.13 | −8.39±0.15 |
| LX Ser | 0.05±0.03 | *−0.21±0.03 | 14.5±0.5 | 14.0±0.1 | 5.1±0.6 | 4.8±0.6 | 0.9±0.2 | 1.4±0.5 | −9.10±0.16 | −8.89±0.19 |
| RW Sex | 0.02±0.02 | −2.01±0.01 | 10.6±0.4 | 10.8±0.1 | 4.3±0.5 | 4.3±0.5 | 4.2±0.7 | 3.9±1.2 | −8.41±0.14 | −8.45±0.17 |
| SW Sex | 0.08±0.02 | −0.97±0.03 | 14.4±0.2 | 13.7±0.1 | 4.3±0.4 | 3.9±0.5 | 3.6±1.1 | 6.3±2.6 | −8.48±0.17 | −8.24±0.21 |
| V3885 Sgr | 0.02±0.02 | −2.12±0.01 | 10.4±0.3 | 10.5±0.1 | 4.8±0.6 | 4.6±0.8 | 3.3±1.5 | 4.1±3.0 | −8.51±0.22 | −8.43±0.33 |
| RW Tri | 0.06±0.02 | −0.77±0.02 | 12.8±0.5 | 13.0±0.1 | 4.4±0.7 | 3.9±0.8 | 1.3±0.6 | 2.3±1.5 | −8.92±0.24 | −8.68±0.31 |
| DW UMa | 0.05±0.03 | *−0.74±0.03 | 14.2±0.3 | 14.0±0.1 | 3.8±0.6 | 3.3±0.7 | 3.1±1.5 | 6.4±4.1 | −8.54±0.24 | −8.23±0.29 |
| UX UMa | 0.02±0.01 | −1.83±0.01 | 12.8±0.6 | 12.9±0.0 | 5.0±0.7 | 4.7±0.7 | 1.9±0.5 | 2.8±1.1 | −8.76±0.16 | −8.59±0.19 |
| IX Vel | 0.02±0.02 | −2.24±0.01 | 9.7±0.4 | 9.8±0.1 | 5.2±0.5 | 5.2±0.6 | 2.6±0.6 | 2.6±1.0 | −8.62±0.15 | −8.62±0.20 |
Notes. This table contains the main results of this study of 42 NLs (Col. 1), i.e. the reddening EB − V (Col. 2), the PL index of the fit to the UV SED (Col. 3), the V magnitude both from the AAVSO data (Col. 4) and from the extrapolation of the UV PL continuum to the V band (after reddening, Col. 5), the i-corrected reference absolute visual magnitude 
(Cols. 6, 7), the i-corrected reference disk luminosity 
(Cols. 8, 9), and the mass accretion Ṁ (Cols. 10, 11). The last three quantities are given for two inclination corrections (see Sect. 7.4). The asterisks indicate objects whose spectral distribution was not an obvious power law (see Sect. 7.1). Subscripts to the quantities in Cols. 6–11 indicate the method used to determine the inclination correction: P for Paczynski & Schwarzenberg-Czerny (1980), W for Webbink et al. (1987). The AAVSO magnitudes are in this table to simplify comparison with the extrapolation of the power law to the V band.
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