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Population synthesis of accreting white dwarfs - II. X-ray and UV emission

文献类型：期刊论文

作者Chen HL(陈海亮)1,2,3,4; Woods, TE2; Yungelson, LR5; Gilfanov, M2,6,7; Han ZW(韩占文)1,3
刊名MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
出版日期2015-11
卷号453期号:3页码:3024-3034
ISSN号0035-8711
关键词binaries: close supernovae: general white dwarfs X-rays: binaries
通讯作者Chen, HL (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
产权排序第一完成单位
英文摘要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.
学科主题Astronomy & Astrophysics
WOS标题词Science & Technology ; Physical Sciences
类目[WOS]Astronomy & Astrophysics
研究领域[WOS]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
收录类别SCI
原文出处http://mnras.oxfordjournals.org/content/453/3/3024
语种英语
WOS记录号WOS:000363649000062
源URL[http://ir.ynao.ac.cn/handle/114a53/4586]  
专题云南天文台_大样本恒星演化研究组
云南天文台_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 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
推荐引用方式
GB/T 7714		 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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