{ "id": "2011.07668", "version": "v1", "published": "2020-11-16T00:52:31.000Z", "updated": "2020-11-16T00:52:31.000Z", "title": "A closer look at non-interacting He stars as a channel for producing the old population of Type Ia supernovae", "authors": [ "Zheng-Wei Liu", "Richard J. Stancliffe" ], "comment": "6 pages, 4 figures, published in Astronomy & Astrophysics (A&A)", "journal": "A&A 641, A20 (2020)", "doi": "10.1051/0004-6361/202038443", "categories": [ "astro-ph.SR" ], "abstract": "The nature of the progenitors of type Ia supernovae (SNe Ia) remains a mystery. Binary systems consisting of a white dwarf (WD) and a main-sequence (MS) donor are potential progenitors of SNe Ia, in which a thermonuclear explosion of the WD may occur when its mass reaches the Chandrasekhar limit during accretion of material from a companion star. In the present work, we address theoretical rates and delay times of a specific MS donor channel to SNe Ia, in which a He star+MS binary produced from a common envelope event subsequently forms a WD+MS system without the He star undergoing mass transfer by Roche lobe overflow. By combining the results of self-consistent binary evolution calculations with population synthesis models, we find that the contribution of SNe Ia in this channel is around 2.0e-4 per year. In addition, we find that delay times of SNe Ia in this channel cover a range of about 1.0-2.6 Gyr, and almost all SNe Ia produced in this way (about 97%) have a delay time of > 1 Gyr. While the rate of SN Ia in this work is about 10% of the overall SN Ia rate, the channel represents a possible contribution to the old population (1-3 Gyr) of observed SNe Ia.", "revisions": [ { "version": "v1", "updated": "2020-11-16T00:52:31.000Z" } ], "analyses": { "keywords": [ "type ia supernovae", "sne ia", "old population", "closer look", "delay time" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 6, "language": "en", "license": "arXiv", "status": "editable" } } }