White-dwarf+main-sequence binaries identified from the tenth data release of Solan Digital Sky Survey [SSA]


We have presented 309 new white-dwarf (WD) + main-sequence (MS) star binaries identified from the Sloan Digital Sky Survey (SDSS) Tenth Data Release (DR10). The majority of them consist of a white dwarf and a low-mass secondary (typically M dwarf) companion. The SDSS spectra of the newly found WDMS binaries with a DA/DB white dwarf and an M/late-K dwarf companion are analyzed based on a spectral decomposition/fitting method. White dwarf effective temperatures, surface gravities and masses together with the secondary star spectral types are obtained, and the stellar parameters of DA WDs with $T_{\rm eff}\la 14,000$ K are revised to the results in the case of 3D model atmosphere. Two independent distance estimates are derived from the flux-scaling factors between the WDMS SDSS spectra and the white dwarf and M-dwarf model spectra. It is found that about more than 20 per cent of the newly found WDMS binaries show a significant discrepancy between the two distance estimates. This might be caused by the effects of M-dwarf stellar activity or irradiation of the M dwarf companions by the white dwarf. The stellar parameter distributions are used to investigate the global properties of newly found WDMS binaries, the results shown in this work are consistent with those derived by previous investigators. Some WDMS binaries have been observed more than one ($2-4$) times by SDSS, it is found that four of them exhibit not only Hydrogen emission in all observable Balmer series lines in addition to He I line Balmer lines but also the rapid variation in the radial velocities of the components in these binaries. This suggests that they should be the post common envelope binaries (PCEBs) with a short orbital period. These young PCEBs are very important for limiting the results of common envelope phase of the binary evolution.

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L. Li, X. Gong, F. Zhang, et. al.
Wed, 10 Dec 14

Comments: 9 pages, 7 figures, 3 tables, submitted to MNRAS