Stellar Wind Accretion and Raman Scattered O VI Features in the Symbiotic Star AG Draconis. (arXiv:1905.05993v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Young-Min Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_H/0/1/0/all/0/1">Hee-Won Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_H/0/1/0/all/0/1">Ho-Gyu Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angeloni_R/0/1/0/all/0/1">Rodolfo Angeloni</a>
We present high resolution spectroscopy of the yellow symbiotic star AG
Draconis with ESPaDOnS at the {it Canada-France-Hawaii Telescope}. Our
analysis is focused on the profiles of Raman scattered ion{O}{VI} features
centered at 6825 AA and 7082 AA, which are formed through Raman scattering
of ion{O}{VI}$lambdalambda$1032 and 1038 with atomic hydrogen. These
features are found to exhibit double component profiles with conspicuously
enhanced red parts. Assuming that the ion{O}{vi} emission region constitutes a
part of the accretion flow around the white dwarf, Monte Carlo simulations for
ion{O}{VI} line radiative transfer are performed to find that the overall
profiles are well fit with the accretion flow azimuthally asymmetric with more
matter on the entering side than on the opposite side. As the mass loss rate of
the giant component is increased, we find that the flux ratio $F(6825)/F(7082)$
of Raman 6825 and 7082 features decreases and that our observational data are
consistent with a mass loss rate $dot Msim 2 times 10^{-7} {rm M_{odot}
yr^{-1}}$. We also find that additional bipolar components moving away with a
speed $sim 70{rm km s^{-1}}$ provide considerably improved fit to the red
wing parts of Raman features. The possibility that the two Raman profiles
differ is briefly discussed in relation to the local variation of the
ion{O}{VI} doublet flux ratio.
We present high resolution spectroscopy of the yellow symbiotic star AG
Draconis with ESPaDOnS at the {it Canada-France-Hawaii Telescope}. Our
analysis is focused on the profiles of Raman scattered ion{O}{VI} features
centered at 6825 AA and 7082 AA, which are formed through Raman scattering
of ion{O}{VI}$lambdalambda$1032 and 1038 with atomic hydrogen. These
features are found to exhibit double component profiles with conspicuously
enhanced red parts. Assuming that the ion{O}{vi} emission region constitutes a
part of the accretion flow around the white dwarf, Monte Carlo simulations for
ion{O}{VI} line radiative transfer are performed to find that the overall
profiles are well fit with the accretion flow azimuthally asymmetric with more
matter on the entering side than on the opposite side. As the mass loss rate of
the giant component is increased, we find that the flux ratio $F(6825)/F(7082)$
of Raman 6825 and 7082 features decreases and that our observational data are
consistent with a mass loss rate $dot Msim 2 times 10^{-7} {rm M_{odot}
yr^{-1}}$. We also find that additional bipolar components moving away with a
speed $sim 70{rm km s^{-1}}$ provide considerably improved fit to the red
wing parts of Raman features. The possibility that the two Raman profiles
differ is briefly discussed in relation to the local variation of the
ion{O}{VI} doublet flux ratio.
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