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| Paper: |
O VI Raman Scattering and the Accretion Disk Emission in the Symbiotic Novae V1016 Cygni and HM Sagittae |
| Volume: |
404, The Eighth Pacific Rim Conference on Stellar Astrophysics: A Tribute to Kam Ching Leung |
| Page: |
82 |
| Authors: |
Lee, H.-W. |
| Abstract: |
The high resolution spectra of the D type symbiotic novae V1016 Cygni and HM Sagittae obtained with the Bohyunsan Optical Echelle Spectrograph (BOES) are presented for the investigation of the double-peaked asymmetric profiles of the Raman scattered O VI 6825. By adopting a wind accretion disk model, the O VI emission region is described by a Keplerian thin disk and the Raman scattering occurs in a neutral region near the giant. Using a Monte Carlo technique, we compute the line profiles that are modulated by the slow spherical stellar wind from the giant component with the ionization front approximated by a hyperboloid. In order to account for the asymmetry and the existence of a central dip in the profiles, we add an O VI resonance scattering region between the hot white dwarf and the giant star which hinders the entrance into the H I region of slightly blue O VI photons. The best fitting parameters for V1016 Cyg are vo = 30 km s-1, v∞ = 11 km s-1, and vc = 10 km s-1, where vo, v∞ and vc are the velocity of the outer disk rim, the terminal velocity of the giant wind, and the velocity component of the resonance scattering O VI region along the binary axis, respectively. Similar fitting parameters vo = 27 km s-1, v∞ = 10 km s-1 and vc = 9 km s-1 are obtained for HM Sge. |
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