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Population synthesis of accreting white dwarfs - II. X-ray and UV emission
Chen HL(陈海亮)1,2,3,4; Woods, TE2; Yungelson, LR5; Gilfanov, M2,6,7; Han ZW(韩占文)1,3
发表期刊MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2015-11
卷号453期号:3页码:3024-3034
DOI10.1093/mnras/stv1865
产权排序第1完成单位
收录类别SCI
关键词Binaries: Close Supernovae: General White Dwarfs X-rays: Binaries
摘要

Accreting white dwarfs (WDs) with non-degenerate companions are expected to emit in soft X-rays and the UV, if accreted H-rich material burns stably. They are an important component of the unresolved emission of elliptical galaxies, and their combined ionizing luminosity may significantly influence the optical line emission from warm interstellar medium (ISM). In an earlier paper, we modelled populations of accreting WDs, first generating WD with main-sequence, Hertzsprung gap and red giant companions with the population synthesis code BSE, and then following their evolution with a grid of evolutionary tracks computed with MESA. Now we use these results to estimate the soft X-ray (0.3-0.7 keV), H- and He II-ionizing luminosities of nuclear burning WDs and the number of supersoft X-ray sources for galaxies with different star formation histories. For the starburst case, these quantities peak at similar to 1 Gyr and decline by similar to 1-3 orders of magnitude by the age of 10 Gyr. For stellar ages of similar to 10 Gyr, predictions of our model are consistent with soft X-ray luminosities observed by Chandra in nearby elliptical galaxies and He II 4686 angstrom/H beta line ratio measured in stacked Sloan Digital Sky Survey spectra of retired galaxies, the latter characterizing the strength and hardness of the UV radiation field. However, the soft X-ray luminosity and He II 4686 angstrom/H beta ratio are significantly overpredicted for stellar ages of less than or similar to 4-8 Gyr. We discuss various possibilities to resolve this discrepancy and tentatively conclude that it may be resolved by a modification of the typically used criteria of dynamically unstable mass-loss for giant stars.

资助项目MPG-CAS Joint Doctoral Promotion Program (DPP) ; Max Planck Institute for Astrophysics (MPA) ; National Natural Science Foundation of China[11521303] ; National Natural Science Foundation of China[11390374] ; Science and Technology Innovation Talent Programme of Yunnan Province[2013HA005] ; Presidium of the Russian Academy of Sciences[P-41] ; RFBR[14-02-00604] ; RFBR[15-02-04053] ; MPA-Garching ; Russian Government Program of Competitive Growth of KFU ; Chinese Academy of Science[XDB09010202]
项目资助者MPG-CAS Joint Doctoral Promotion Program (DPP) ; Max Planck Institute for Astrophysics (MPA) ; National Natural Science Foundation of China[11521303, 11390374] ; Science and Technology Innovation Talent Programme of Yunnan Province[2013HA005] ; Presidium of the Russian Academy of Sciences[P-41] ; RFBR[14-02-00604, 15-02-04053] ; MPA-Garching ; Russian Government Program of Competitive Growth of KFU ; Chinese Academy of Science[XDB09010202]
语种英语
学科领域天文学 ; 恒星与银河系 ; 恒星形成与演化
学科门类理学 ; 理学::天文学
文章类型Article
出版者OXFORD UNIV PRESS
出版地GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
归档日期2015-11-24
WOS记录号WOS:000363649000062
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]EARLY-TYPE GALAXIES ; COMMON-ENVELOPE EVOLUTION ; APPROXIMATE LAMBDA OPERATORS ; STELLAR ASTROPHYSICS MESA ; STAR-FORMATION HISTORIES ; DELAY-TIME DISTRIBUTION ; HYDROGEN SHELL FLASHES ; INITIAL MASS FUNCTION ; IA SUPERNOVA RATE ; MODEL ATMOSPHERES
引用统计
被引频次:29[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/4586
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
通讯作者Chen HL(陈海亮)
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
2.Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, Garching b. München D-85741, Germany
3.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
4.University of Chinese Academy of Sciences, Beijing 100049, China
5.Institute of astronomy, RAS, 48 Pyatnitskaya Str., 119017 Moscow, Russia
6.Space Research Institute of Russian Academy of Sciences, Profsoyuznaya 84/32,117997 Moscow, Russia
7.Kazan Federal University, Kremlevskaya str.18, 420008 Kazan, Russia
第一作者单位中国科学院云南天文台
通讯作者单位中国科学院云南天文台
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Chen HL,Woods, TE,Yungelson, LR,et al. Population synthesis of accreting white dwarfs - II. X-ray and UV emission[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2015,453(3):3024-3034.
APA Chen HL,Woods, TE,Yungelson, LR,Gilfanov, M,&Han ZW.(2015).Population synthesis of accreting white dwarfs - II. X-ray and UV emission.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,453(3),3024-3034.
MLA Chen HL,et al."Population synthesis of accreting white dwarfs - II. X-ray and UV emission".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 453.3(2015):3024-3034.
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