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Paper: Raman Scattering and Accretion Disks in Symbiotic Stars
Volume: 289, The Proceedings of the IAU 8th Asian-Pacific Regional Meeting, Volume I
Page: 281
Authors: Lee, Hee-Won
Abstract: Symbiotic stars are generally known to be well-detached systems of a mass-losing giant and a hot white dwarf. It has been suspected that some fraction of the slow stellar wind from the giant component may be captured by the white dwarf component forming an accretion disk. Here, it is argued that in symbiotic stars the existence of an accretion disk is strongly implied by the characteristic features exhibited by the Raman-scattered O~VI lines around 6830 A and 7088 A. Double of triple-peaked profiles in the Raman-scattered lines and single-peak profiles in other emission lines are interpreted as line-of-sight effects, where H I scatterers near the giant view an incident double-peaked profile and an observer with a low inclination sees single-peak profiles. In this accretion disk model, it is proposed that an inhomogeneous mass concentration around the accretion disk formed by a dusty wind may lead to the disparate ratios of the blue peak strength to the red counterpart observed in the 6830 A and 7088 A features. We present a (Canada-France-Hawaii Telescope) CFHT spectrum of the symbiotic star V1016 Cyg, which supports the accretion disk model.
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