The AM Canum Venaticorum (AM CVn) binaries are a rare group of hydrogen-deficient, ultra-short period, mass-transferring white dwarf binaries, and are possible progenitors of type Ia supernovae. We present time-resolved spectroscopy of the recently-discovered AM CVn binary SDSS J173047.59+554518.5. The average spectrum shows strong double-peaked helium emission lines, as well as a variety of metal lines, including neon; this is the second detection of neon in an AM CVn binary, after the much brighter system GP Com. We detect no calcium in the accretion disc, a puzzling feature that has been noted in many of the longer-period AM CVn binaries. We measure an orbital period, from the radial velocities of the emission lines, of 35.2 +/- 0.2 minutes, confirming the ultra-compact binary nature of the system. The emission lines seen in SDSS J1730 are very narrow, although double-peaked, implying a low inclination, face-on accretion disc; using the measured velocities of the line peaks, we estimate i < 11 degrees. This low inclination makes SDSS J1730 an excellent system for the identification of emission lines.
@article{arxiv.1311.0008,
title = {The AM CVn binary SDSS J173047.59+554518.5},
author = {P. J. Carter and D. Steeghs and T. R. Marsh and T. Kupfer and C. M. Copperwheat and P. J. Groot and G. Nelemans},
journal= {arXiv preprint arXiv:1311.0008},
year = {2015}
}
Comments
8 pages, 6 figures, 3 tables. Accepted for publication in MNRAS