2001/03/21 by Maria Teresa Ruiz, M. T. Ruíz, Patricio M. Rojo +4 · 7 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/320578
Astrophysical Journal, 20 pages
arxiv created 2001/03/21 · openalex publication_date 2001/05/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We present spectroscopic observations of object CE 315 revealing a blue continuum with strong emission lines. Most of the detected lines are identified with He I or He II in emission, with a handful of faint lines of nitrogen. Notable is the complete absence of hydrogen lines. The He lines exhibit triple-peaked profiles with remarkably broad widths of ~2000 km s -1 (FWZP). The observations show that CE 315 is an interacting binary system with an orbital period of 65.1 ± 0.7 minutes and a mass ratio of 0.022. We conclude that the most likely scenario for this object is that of an accreting ~0.77 M ☉ white dwarf with a ~0.017 M ☉ helium white dwarf as mass donor.