Emission Line Flickering from the Secondary Star in Cataclysmic Variables? A study of V3885 Sagitarii
Feb, 200719 pages
Published in:
- Astron.J. 133 (2007) 2659-2668
e-Print:
- astro-ph/0702308 [astro-ph]
DOI:
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Abstract: (arXiv)
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.- accretion, accretion disks
- binaries: close
- novae, cataclysmic variables
- stars: individual (V3885 Sagittarii)
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