Emission Line Flickering from the Secondary Star in Cataclysmic Variables? A study of V3885 Sagitarii
arXiv:astro-ph/0702308 · doi:10.1086/514335
Abstract
Spectrophotometric observations of H-alpha and He I 6678 emission lines of the nova-like Cataclysmic Variable V3885 Sgr are presented and analyzed. The binary orbital period was determined as P = 0.20716071(22) days. Doppler Tomography was performed with both H-alpha and He I lines. Disc radial emissivity profiles were also computed. The tomography mapping of flickering sources was performed using the H-alpha line, from which we concluded that the flickering is not uniformly distributed on the disc. The observed tomogram of the flickering was compared with simulations, suggesting that the most intense flickering source in the H-alpha is not located in the accretion disc. It is proposed that the main line flickering source may be associated with the illuminated secondary star.
19 pages, 10 figures, 1 table. Accepted to be published on AJ. to donwload high resolution figures: http://www.astro.iag.usp.br/~fabiola/V3885_hires.pdf
References in corpus (4)
Cited by in corpus (9)
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- A MeerKAT Survey of Nearby Novalike Cataclysmic Variables
- Novalike Cataclysmic Variables in the Infrared
- Analysis of the white--light flickering of the Intermediate Polar V709 Cas with wavelets and Hurst analysis
- Tomographic Simulations of Accretion Disks in Cataclysmic Variables - Flickering and Wind
- Orbital and stochastic far-UV variability in the nova-like system V3885 Sgr
- A search and modeling of peculiar narrow transient line components in novae spectra
- A Time-Series Analysis of the H-alpha Emission Line in V3885 Sagitarii