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Reference: Liu, D-D, Wang, B, Podsiadlowski, P et al., (2016). The violent white dwarf merger scenario for the progenitors of Type Ia supernovae. Monthly Notices of the Royal Astronomical Society, 461 (4), 3653-3662.Citable link to this page:

 

The violent white dwarf merger scenario for the progenitors of Type Ia supernovae

Abstract: Recent observations suggest that some Type Ia supernovae (SNe Ia) originate from the merging of two carbon-oxygen white dwarfs (CO WDs). Meanwhile, recent hydrodynamical simulations have indicated that the accretion-induced collapse may be avoided under certain conditions when double WDs merge violently. However, the properties of SNe Ia from this violent merger scenario are highly dependent on a particular mass-accretion stage, the so-called WD + He subgiant channel, during which the primary WD is able to increase its mass by accreting He-rich material from an He subgiant before the systems evolves into a doubleWD system. In this paper, we aim to study this particular evolutionary stage systematically and give the properties of violentWDmergers. By employing the Eggleton stellar evolution code, we followed a large number of binary calculations and obtained the regions in parameter space for producing violent mergers based on the WD + He subgiant channel. According to these simulations, we found that the primary WDs can increase their mass by ∼0.10-0.45M⊙ during the massaccretion stage. We then conducted a series of binary population synthesis calculations and found that the Galactic SN Ia birthrate from this channel is about 0.01-0.4 × 10-3 yr-1. This suggests that the violent WD mergers from this channel may only contribute to ∼0.3-10 per cent of all SNe Ia in our Galaxy. The delay times of violent WD mergers from this channel are ≥1.7Gyr, contributing to the SNe Ia in old populations. We also found that the WD + He subgiant channel is the dominant way for producing violent WD mergers that may be able to eventually explode as SNe Ia.

Publication status:PublishedPeer Review status:Peer reviewedVersion:Publisher's version Funder: National Basic Research Program of China   Funder: National Natural Science Foundation of China   Funder: Chinese Academyof Sciences   Funder: NaturalScience Foundation of Yunnan Province   Funder: Youth Innovation PromotionAssociation CAS   Notes:Copyright © 2016 the Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

Bibliographic Details

Publisher: Oxford University Press

Publisher Website: http://www.oxfordjournals.org/

Journal: Monthly Notices of the Royal Astronomical Societysee more from them

Publication Website: http://mnras.oxfordjournals.org/

Volume: 461

Issue: 4

Extent: 3653-3662

Issue Date: 01 October 2016

pages:3653-3662Identifiers

Doi: https://doi.org/10.1093/mnras/stw1575

Eissn: 1365-2966

Issn: 0035-8711

Uuid: uuid:41b8d334-f166-459a-9510-f9ecf6a36bf3

Urn: uri:41b8d334-f166-459a-9510-f9ecf6a36bf3

Pubs-id: pubs:634411 Item Description

Type: journal-article;

Version: Publisher's versionKeywords: binaries: close stars: evolution supernovae: general white dwarfs

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Autor: Liu, D-D - - - Wang, B - - - Podsiadlowski, P - Oxford, MPLS, Physics, Astrophysics St Edmund Hall - - - Han, Z - - - - Bibliogra

Fuente: https://ora.ox.ac.uk/objects/uuid:41b8d334-f166-459a-9510-f9ecf6a36bf3



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