Emission-Line Flickering from the Secondary Star in Cataclysmic Variables? A Study of V3885 Sagittarii | Zendy

Fabíola Mariana Aguiar Ribeiro | Zendy; Marcos P. Diaz | Zendy

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Emission-Line Flickering from the Secondary Star in Cataclysmic Variables? A Study of V3885 Sagittarii

Author(s) -

Fabíola Mariana Aguiar Ribeiro,

Marcos P. Diaz

Publication year - 2007

Publication title -

the astronomical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.61

H-Index - 271

eISSN - 1538-3881

pISSN - 0004-6256

DOI - 10.1086/514335

Subject(s) - physics , astrophysics , flicker , cataclysmic variable star , dwarf nova , line (geometry) , astronomy , emission spectrum , orbital period , spectral line , stars , white dwarf , geometry , mathematics , electrical engineering , engineering

Spectrophotometric observations of H-alpha and He I 6678 emission lines ofthe nova-like Cataclysmic Variable V3885 Sgr are presented and analyzed. Thebinary orbital period was determined as P = 0.20716071(22) days. DopplerTomography was performed with both H-alpha and He I lines. Disc radialemissivity profiles were also computed. The tomography mapping of flickeringsources was performed using the H-alpha line, from which we concluded that theflickering is not uniformly distributed on the disc. The observed tomogram ofthe flickering was compared with simulations, suggesting that the most intenseflickering source in the H-alpha is not located in the accretion disc. It isproposed that the main line flickering source may be associated with theilluminated secondary star.

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