Spectroscopic evidence for the binary nature of AM CVn
نویسندگان
چکیده
منابع مشابه
The AM CVn binary SDSSJ173047.59+554518.5
The AM Canum Venaticorum (AM CVn) binaries are a rare group of hydrogendeficient, 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 met...
متن کاملAM CVn stars
I review our observational and theoretical knowledge of AM CVn stars, focusing on recent developments. These include newly discovered systems, the possibility that two recently discovered extremely short period objects are AM CVn stars and an update on X-ray, UV an optical studies. Theoretical advances include the study of the details of both the donor and accretor, and the physics of the heliu...
متن کاملThe outburst properties of AM CVn stars
We briefly summarize the observational properties of ultra-compact binaries called AM CVn stars. We analize their outbursts originating from the thermal-viscous instability in helium accretion disc. We present our preliminary results in applying the model of Dwarf Novae outbursts to helium discs. We can calculate models of outbursts of reasonable amplitude of 2 mag with a constant α parameter t...
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We report the results of a synthetic spectral analysis of Hubble STIS spectra of the AM CVn-type cataclysmic variable CP Eri obtained when the system was in quiescence. The FUV spectrum is best fitted by a helium-dominated, hybrid composition (DBAZ) white dwarf with Teff ∼ 17, 000K ± 1000K, log g∼ 8, He abundance ∼ 1000× solar, H abundance ∼ 0.1× solar, metallicity Z ∼ 0.05× solar, V sin i ∼ 40...
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High speed photometry of the new AM CVn star in Hya (previously known as SN2003aw), spectroscopically identified by Chornock & Filippenko, shows it to have a superhump period of 2041.5 ± 0.3 s. We find a range of brightness from V ∼ 16.5 to 20.3, presumably caused by variations in the rate of mass transfer. In the intermediate state the system cycles in brightness with a period of ∼ 16 h and ra...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2001
ISSN: 0035-8711,1365-2966
DOI: 10.1046/j.1365-8711.2001.04614.x