Table A.1
Observational data of a number of low-mass He WDs (and proto-He WDs), preferentially in tight binary systems.
| He WD | log g(cm s-2) | Teff (K) | MWD(M⊙) | Porb (h) | Optical data |
|
|
|||||
| PSR J0337+1715 | 5.82 ± 0.05 | 15 800 ± 100 | 0.197 ± 0.0002 | 39.12 | Kaplan et al. (2014b) |
| PSR J0348+0432 | 6.035 ± 0.06 | 10 120 ± 90 | 0.172 ± 0.003 | 2.46 | Antoniadis et al. (2013) |
| PSR J0751+1807 | 7.41 ± 0.48 | 3900 ± 400 | 0.138 ± 0.0006 a | 6.31 | Bassa et al. (2006b) |
| PSR J1012+5307 | 6.75 ± 0.07 | 8550 ± 25 | 0.16 ± 0.02 | 14.51 | van Kerkwijk et al. (1996); Callanan et al. (1998) |
| PSR J1738+0333 | 6.45 ± 0.07 | 9130 ± 150 | 0.182 ± 0.016 | 8.52 | Antoniadis et al. (2012) |
| PSR J1816+4510 | 4.9 ± 0.3 | 16 000 ± 500 | ~ 0.21 ± 0.02 b | 8.66 | Kaplan et al. (2012, 2013) |
| PSR J1909−3744 | 6.77 ± 0.04 | 9050 ± 50 | 0.2038 ± 0.0022 | 36.72 | Antoniadis (2013) |
| PSR J0024−7204Uc | ~5.6 | ~ 11 000 | ~ 0.17 | 10.29 | Edmonds et al. (2001) |
| PSR J1911−5958Ac | 6.44 ± 0.20 | 10 090 ± 150 | 0.175 ± 0.010 | 20.64 | Bassa et al. (2006a) |
|
|
|||||
| NLTT 11748 | 6.35 ± 0.03 | 7600 ± 120 | 0.149 ± 0.013 | 5.64 | Kaplan et al. (2014a) |
|
|
|||||
| KOI−74 | 6.51 ± 0.14 | 13 000 ± 1000 | 0.22 ± 0.03 | 125.53 | van Kerkwijk et al. (2010) |
| KOI−1224 | 5.75 ± 0.06 | 14 700 ± 1000 | 0.22 ± 0.02 | 64.75 | Breton et al. (2012) |
| KIC 10657664 | 5.50 ± 0.02 | 14 600 ± 300 | 0.26 ± 0.04 d | 78.55 | Carter et al. (2011) |
|
|
|||||
| SDSS J184037.78 | 6.49 ± 0.06 | 9390 ± 140 | ~ 0.17 | 4.59 | Hermes et al. (2013) e,f |
| SDSS J111215.82 | 6.36 ± 0.06 | 9590 ± 140 | ~ 0.17 | 4.14 | Hermes et al. (2013) e,f |
| SDSS J151826.68 | 6.90 ± 0.05 | 9900 ± 140 | ~ 0.23 | 14.62 | Hermes et al. (2013) e,f |
| J1614 | 6.66 ± 0.14 | 8800 ± 170 | ~ 0.19 | – | Hermes et al. (2013) f |
| J2228 | 6.03 ± 0.08 | 7870 ± 120 | ~ 0.16 | – | Hermes et al. (2013) f |
Notes.
Based on Kaplan et al. (2013). See also Istrate et al. (2014) for further comments on the component masses of this source.
The WD is most likely to have formed in this globular cluster binary given that the eccentricity is e< 10-5, as expected from recycling.
Carter et al. (2011) found two possible solutions for MWD (0.26 M⊙ and 0.37 M⊙). This WD has Porb = 3.3 days and thus we adopt the lower value of MWD since this is agrees much better with the known (MWD,Porb)-correlation (see Tauris & Savonije 1999, for discussions).
Pulsating He WDs, see Córsico & Althaus (2014) for recent theoretical modelling.
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