Evolution of double oxygen-neon white dwarf merger remnant

doi:10.1093/mnras/stad2636

YNAO OpenIR > 大样本恒星演化研究组

	Evolution of double oxygen-neon white dwarf merger remnant
	Wu CY(吴程远)1,2,3 ; Xiong, Heran 4; Han ZW(韩占文)1,2,3 ; Wang B(王博)1,2,3
发表期刊	MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
	2023-09-11
卷号	525 期号:4 页码:6295-6302
DOI	10.1093/mnras/stad2636
产权排序	第1完成单位
收录类别	SCI ; EI
关键词	binaries: close stars: evolution supernovae: general white dwarfs
摘要	Double white dwarf (WD) merger process and their post-merger evolution are important in many fields of astronomy, such as supernovae, gamma-ray bursts, gravitational waves, and so on. The evolutionary outcomes of double ultra-massive WD merger remnants are still a subject of debate, though the general consensus is that the merger remnant will collapse to form a neutron star (NS). In this work, we investigate the evolution of a 2.20M(circle dot) merger remnant stemmed from the coalescence of double 1.10M(circle dot) ONe WDs. We find that the remnant ignites off-centre neon burning at the position near the surface of primary WD soon after the merger, resulting in the stable inwardly propagating oxygen/neon (O/Ne) flame. The final outcomes of the merger remnant are sensitive to the effect of convective boundary mixing. If the mixing cannot stall the O/Ne flame, the flame will reach the centre within 20 yr, leading to the formation of super Chandrasekhar mass silicon core, and its final fate probably be NS through iron-core-collapse supernova. In contrast, if the convective mixing is effective enough to prevent the O/Ne flame from reaching the centre, the merger remnant will undergo electron capture supernova to form an ONeFe WD. Meanwhile, we find that the wind mass loss process may hardly alter the final fate of the remnant due to its fast evolution. Our results imply that the coalescence of double ONe WDs can form short lived giant like object, but the final outcomes (NS or ONeFe WD) are influenced by the uncertain convective mixing in O/Ne flame.
资助项目	National Natural Science Foundation of China[12288102]; National Natural Science Foundation of China[12003013]; National Natural Science Foundation of China[12225304]; National Natural Science Foundation of China[12333008]; National Natural Science Foundation of China[2021YFA1600404]; National Key R&D Program of China[XBZG-ZDSYS-202117]; Western Light Project of CAS[CMS-CSST-2021-A12]; China Manned Space Project[202301AU070039]; China Manned Space Project[202001AS070029]; China Manned Space Project[202201BC070003]; Yunnan Fundamental Research Projects[2022-QYKYJH-ZYTS-016]; Frontier Scientific Research Program of Deep Space Exploration Laboratory[202302AN360001]; International Centre of Supernovae, Yunnan Key Laboratory
项目资助者	National Natural Science Foundation of China[12288102, 12003013, 12225304, 12333008] ; National Natural Science Foundation of China[2021YFA1600404] ; National Key R&D Program of China[XBZG-ZDSYS-202117] ; Western Light Project of CAS[CMS-CSST-2021-A12] ; China Manned Space Project[202301AU070039, 202001AS070029, 202201BC070003] ; Yunnan Fundamental Research Projects[2022-QYKYJH-ZYTS-016] ; Frontier Scientific Research Program of Deep Space Exploration Laboratory[202302AN360001] ; International Centre of Supernovae, Yunnan Key Laboratory
语种	英语
学科领域	天文学
文章类型	Article
出版者	OXFORD UNIV PRESS
出版地	GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN	0035-8711
URL	查看原文
WOS记录号	WOS:001183266000043
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	GAMMA-RAY-BURST ; AFTERGLOW LIGHT CURVES ; EXTENDED EMISSION ; OPTICAL/NIR AFTERGLOW ; DURATION DISTRIBUTION ; INTRINSIC DURATIONS ; FUNDAMENTAL PLANE ; ENERGY INJECTION ; CENTRAL ENGINE ; FERMI-LAT
EI入藏号	20234515007193
EI主题词	Oxygen
EI分类号	657.2 Extraterrestrial Physics and Stellar Phenomena - 801.3 Colloid Chemistry - 802.3 Chemical Operations - 804 Chemical Products Generally - 931.3 Atomic and Molecular Physics - 932.1 High Energy Physics
引用统计
文献类型	期刊论文
条目标识符	http://ir.ynao.ac.cn/handle/114a53/26491
专题	大样本恒星演化研究组中国科学院天体结构与演化重点实验室
作者单位	1.Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650216, China; 2.Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, CAS, Kunming, 650216, China; 3.International Centre of Supernovae, Yunnan Key Laboratory, Kunming, 650216, China; 4.Research School of Astronomy and Astrophysics, The Australian National University, Canberra, ACT, 2611, Australia
第一作者单位	中国科学院云南天文台
推荐引用方式 GB/T 7714	Wu CY,Xiong, Heran,Han ZW,et al. Evolution of double oxygen-neon white dwarf merger remnant[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2023,525(4):6295-6302.
APA	吴程远,Xiong, Heran,韩占文,&王博.(2023).Evolution of double oxygen-neon white dwarf merger remnant.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,525(4),6295-6302.
MLA	吴程远,et al."Evolution of double oxygen-neon white dwarf merger remnant".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 525.4(2023):6295-6302.

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