Formation and Evolution of Ultraluminous X-Ray Pulsar Binaries to Pulsar-Neutron Star and Pulsar-White Dwarf Systems

doi:10.3847/1538-4357/abb5a8

	Formation and Evolution of Ultraluminous X-Ray Pulsar Binaries to Pulsar-Neutron Star and Pulsar-White Dwarf Systems
	Abdusalam, K.6; Ablimit, Iminhaji 4,5; Hashim, P.3; Lü, G. -L.2,6; Mardini, M. K.1,5; Wang, Z. -J.6
刊名	The Astrophysical Journal
	2020-10-01
卷号	902 页码:125
关键词	Binary stars Close binary stars X-ray binary stars Pulsars Gravitational wave sources White dwarf stars Compact objects 154 254 1811 1306 677 1799 288 Astrophysics - High Energy Astrophysical Phenomena
ISSN号	0004-637X
DOI	10.3847/1538-4357/abb5a8
产权排序	4
英文摘要	Recent observational and theoretical results have suggested that some of ultraluminous X-ray (ULX) sources may contain neutron star (NS) accretors. However, the formation channel and properties of donor stars of NS ULXs remain uncertain. By adopting the nonconservative and rotation-dependent mass transfer model in the primordial binary evolution, we investigate the way to form pulsar ULXs like observed pulsar ULXs in a systematic way. Our simulation results indicate that pulsar ULXs with Be stars and intermediate or/and high-mass donors match observed apparent luminosities, orbital periods, and observationally indicated donor masses of known pulsar ULXs. ULXs with Be and intermediate donors are main contributors. The route of accretion-induced collapse of WDs has a 4.5% contribution to the NS ULXs, 4.0% of NSs in ULXs are formed through electron-capture supernovae (SNe), and 91.5% of NSs in ULXs are born with core-collapse SNe. We also studied the evolution of pulsar ULXs to double compact star systems. We do not find NS-black hole systems (merging in a Hubble time) that evolved from pulsar ULXs. Pulsar-white dwarf (WD) cases that evolve through pulsar ULXs have significant contributions to the whole NS-WD gravitational wave sources. Contributions of pulsar-WD and pulsar-NS cases that experienced pulsar ULXs are ∼40% and 11% among all LISA NS-WD and NS-NS sources, respectively. Monte Carlo simulation noise with different models give a nonnegligible uncertainty.
URL标识	查看原文
语种	英语
内容类型	期刊论文
源URL	[http://ir.xao.ac.cn/handle/45760611-7/4065]
专题	新疆天文台_光学天文与技术应用研究室
作者单位	1.Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, People’s Republic of China 2.Center for Theoretical Physics, Xinjiang University, Urumqi 830046, People’s Republic of China; 3.Astronomical Observatory of Xinjiang, Chinese Academy of Sciences, Urumqi 830046, People’s Republic of China; 4.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan; 5.Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People’s Republic of China; 6.School of Physical Science and Technology, Xinjiang University, Urumqi 830046, People’s Republic of China;
推荐引用方式 GB/T 7714	Abdusalam, K.,Ablimit, Iminhaji,Hashim, P.,et al. Formation and Evolution of Ultraluminous X-Ray Pulsar Binaries to Pulsar-Neutron Star and Pulsar-White Dwarf Systems[J]. The Astrophysical Journal,2020,902:125.
APA	Abdusalam, K.,Ablimit, Iminhaji,Hashim, P.,Lü, G. -L.,Mardini, M. K.,&Wang, Z. -J..(2020).Formation and Evolution of Ultraluminous X-Ray Pulsar Binaries to Pulsar-Neutron Star and Pulsar-White Dwarf Systems.The Astrophysical Journal,902,125.
MLA	Abdusalam, K.,et al."Formation and Evolution of Ultraluminous X-Ray Pulsar Binaries to Pulsar-Neutron Star and Pulsar-White Dwarf Systems".The Astrophysical Journal 902(2020):125.