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Abstract: We compute the remaining amounts of hydrogen in red giant donors to seewhether the conflict between theory and observations can be overcome. Byconsidering the mass-stripping effect from an optically thick wind and theeffect of thermally unstable disk, we systematically carried out binaryevolution calculation for WD + MS and WD + RG systems. Here, we focus on theevolution of WD + RG systems. We found that some donor stars at the time of thesupernova explosion contain little hydrogen-rich material on top of the heliumcore as low as 0.017 $M {\odot}$, which is smaller than the upper limit tothe amount derived from observations of material stripped-off by explosionejecta. Thus, no hydrogen line is expected in the nebular spectra of these SNIa. We also derive the distributions of the envelope mass and the core mass ofthe companions from WD + RG channel at the moment of a supernova explosion byadopting a binary population synthesis approach. We rarely find a RG companionwith a very low-mass envelope. Furthermore, our models imply that the remnantof the WD + RG channel emerging after the supernova explosion is a singlelow-mass white dwarf 0.15 $M {\odot}$ - 0.30 $M {\odot}$. The absence of ahydrogen line in nebular spectra of SNe Ia provides support to the proposalthat the WD + RG system is the progenitor of SNe Ia.



Autor: Xiangcun Meng, Wuming Yang

Fuente: https://arxiv.org/



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