1. Raman-scattered O VI λ1032 and He II λ1025 and Bipolar Outflow in the Symbiotic Star V455 Sco
- Author
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Jeong-Eun Heo, Chae-Lin Hong, Tali Palma, Rodolfo Angeloni, Seok-Jun Chang, Francesco Di Mille, and Hee-Won Lee
- Subjects
History ,010504 meteorology & atmospheric sciences ,Hydrogen ,Lyman series ,Astrophysics::High Energy Astrophysical Phenomena ,chemistry.chemical_element ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Spectral line ,Computer Science Applications ,Education ,symbols.namesake ,Stars ,chemistry ,Symbiotic star ,Mass transfer ,Bipolar outflow ,0103 physical sciences ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Raman spectroscopy ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences - Abstract
Raman-scattering by atomic hydrogen is a unique spectroscopic process that may probe the mass transfer and mass loss phenomena in symbiotic stars(SSs). In the optical high- resolution spectra of the S-type SS V455 Sco, we note the presence of two Raman-scattered features, one at around 6825 A with a triple-peak profile formed from Raman-scattering of O VI λ1032 and the other Raman-scattered He II λ1025 at around 6545 A. Adopting an accretion flow model with additional contribution from a collimated bipolar outflow, we propose that the blue and central peaks are contributed from the accretion flow and the bipolar flow is responsible for the remaining red peak. With the absence of [N II] λ6548, the Raman-scattered He II λ1025 at around 6545 A is immersed in the broad Ha wings that appear to be formed by Raman-scattering of far-UV continuum near Lyman series.
- Published
- 2016
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