2015/10/21 by Matej Sekeráš, M. Sekeráš, A. Skopal +1 · 3 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Binary number #Constraint (computer-aided design) #Raman scattering #Raman spectroscopy #Scattering #Scattering rate #Scientific Research and Discoveries #Spectral line #Stellar, planetary, and galactic studies #Symbiotic star #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/812/2/162
published as Astrophysical Journal 812, 162 (2015) · 8 pages, 8 figures, 2 tables
openalex publication_date 2015/10/21 · arxiv created 2015/10/28 · arxiv updated 2015/10/29 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The mass-loss rate from Mira variables represents a key parameter in our understanding of their evolutionary tracks. We introduce a method for determining the mass-loss rate from the Mira component in D-type symbiotic binaries via the Raman scattering of atomic hydrogen in the wind from the giant. Using our method, we investigated Raman He ii conversion in the spectrum of the symbiotic Mira V1016 Cyg. We determined its efficiency, η = 0.102, 0.148, and the corresponding mass-loss rate, , using our spectra from 2006 April and 2007 July, respectively. Our values of that we derived from Raman scattering are comparable with those obtained independently by other methods. Applying the method to other Mira–white dwarf binary systems can provide a necessary constraint in the calculation of asymptotic giant branch (AGB) evolution.