The AM Canum Venaticorum binary SDSS J173047.59+554518.5

P. J. Carter*, D. Steeghs, T. R. Marsh, T. Kupfer, C. M. Copperwheat, P. J. Groot, G. Nelemans

*Corresponding author for this work

Research output: Contribution to journalArticle (Academic Journal)peer-review

13 Citations (Scopus)

Abstract

The AM Canum Venaticorum (AM CVn) binaries are a rare group of hydrogen-deficient, ultrashort 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 min, confirming the ultracompact 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.

Original languageEnglish
Pages (from-to)2894-2900
Number of pages7
JournalMonthly Notices of the Royal Astronomical Society
Volume437
Issue number3
DOIs
Publication statusPublished - Jan 2014

Keywords

  • accretion
  • accretion discs
  • binaries: close
  • stars: individual: SDSS J173047
  • 59+554518.5
  • novae,cataclysmic variables
  • white dwarfs
  • DIGITAL-SKY-SURVEY
  • CVN STARS
  • ORBITAL PERIOD
  • ACCRETION DISKS
  • WHITE-DWARF
  • POPULATION
  • CANDIDATES
  • EMISSION
  • SYSTEMS
  • SUPERNOVAE

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