SIMBAD references

2014MNRAS.437.2894C - Mon. Not. R. Astron. Soc., 437, 2894-2900 (2014/January-3)

The AM Canum Venaticorum binary SDSS J173047.59+554518.5.

CARTER P.J., STEEGHS D., MARSH T.R., KUPFER T., COPPERWHEAT C.M., GROOT P.J. and NELEMANS G.

Abstract (from CDS):

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±0.2min, 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°. This low inclination makes SDSS J1730 an excellent system for the identification of emission lines.

Abstract Copyright: © The Authors 2013. Published by Oxford University Press on behalf of The Royal Astronomical Society. (2013)

Journal keyword(s): accretion, accretion discs - binaries: close - stars: individual: SDSS J173047.59+554518.5 - novae, cataclysmic variables - white dwarfs

Simbad objects: 10

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2014MNRAS.437.2894C and select 'bookmark this link' or equivalent in the popup menu


2021.05.17-11:52:38

© Université de Strasbourg/CNRS

    • Contact