Stellar Wind Accretion and Raman O VI Spectroscopy of the Symbiotic Star AG Draconis

Abstract Raman scattered O VI features at 6825 Å and 7082 Å found in symbiotic stars are important spectroscopic tools to probe the mass transfer process. Adopting a Monte Carlo approach, we perform a profile analysis of Raman O VI features of the yellow SySt AG Draconis and make a comparison with t...

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Published inProceedings of the International Astronomical Union Vol. 14; no. S343; pp. 449 - 451
Main Authors Lee, Young-Min, Heo, Jeong-Eun, Lee, Hee-Won, Lee, Ho-Gyu, Angeloni, Rodolfo, Di Mille, Francesco, Palma, Tali
Format Journal Article
LanguageEnglish
Published Cambridge Cambridge University Press 01.08.2018
Subjects
Accretion
Astronomy
Binary stars
Computer simulation
Deposition
Emissions
Mass transfer
Spectrum analysis
Stellar winds
Symbiotic stars
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Summary:Abstract Raman scattered O VI features at 6825 Å and 7082 Å found in symbiotic stars are important spectroscopic tools to probe the mass transfer process. Adopting a Monte Carlo approach, we perform a profile analysis of Raman O VI features of the yellow SySt AG Draconis and make a comparison with the spectrum obtained with CFHT. It is assumed that the accretion flow is convergent on the entering side with enhanced O VI emission and the flux ratio F (1032)/ F (1038)∼1, whereas on the opposite side the flow is divergent with low O VI emission and F (1032/ F (1038)∼2. Our best fit to the spectrum is obtained from our model with a mass-loss rate of the giant ∼4 × 10 −7 M ⊙ yr −1 . A slight red wing excess in the spectrum suggests the presence of bipolar neutral components receding in the directions perpendicular to the binary orbital plane with a speed ∼70km s −1
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921318006130