YNAO OpenIR  > 大样本恒星演化研究组
Formation of hot subdwarf B stars with neutron star components
Wu Y(吴优)1,2,3; Chen XF(陈雪飞)1,2,4; Li ZW(李振威)1,2,3; Han ZW(韩占文)1,2,4
Source PublicationASTRONOMY & ASTROPHYSICS
2018-10-05
Volume618Pages:12
DOI10.1051/0004-6361/201832686
Contribution Rank第1完成单位
Indexed BySCI ; EI
KeywordBinaries: General Stars: Formation Stars: Neutron Subdwarfs
Abstract

Context. Binary population synthesis predicts the existence of subdwarf B stars (sdBs) with neutron star (NS) or black hole (BH) companions. Several works have been dedicated to finding such systems, but none has been confirmed yet. Theoretically, the formation of sdBs with white dwarf (WD) and main sequence (MS) companions has been well investigated, while those with NS or BH companions remain to be explored further. 

Aims. We systematically investigate the formation of sdB + NS binaries from binary evolution and aim to obtain some clues for a search for such systems. 

Methods. We started from a series of MS + NS systems and determined the parameter spaces for producing sdB + NS binaries from the stable Roche-lobe overflow (RLOF) channel and from the common envelope (CE) ejection channel. The parameters for sdB + NS binaries were obtained from detailed binary evolution calculation with the code called modules for experiments in stellar astrophysics (MESA), and the CE parameters were given by the standard energy budget for CE evolution. The MS star had an initial mass ranging from 0.8 to 5 M fi. Various NS accretion e ffi ciencies and NS masses were examined to investigate the e ff ects they have. We show the characteristics of the produced sdB + NS systems, such as the mass of components, orbital period, the semi-amplitude of the radial velocity (K), and the spin of the NS component. 

Results. sdB + NS binaries can be produced either from stable RLOF or from CE ejection. In the stable RLOF channel, sdBs can be formed when the donor starts mass transfer close to the tip of the giant branch if the donor has an initial mass similar to 2 : 0 M fi. For more massive donors, sdBs can be formed when the donor starts mass transfer during the Hertzsprung gap or near the end of the MS. The orbital period of sdB + NS binaries produced in this way ranges from several days to more than 1000 days and moves toward the short-period (similar to hr) side with increasing initial MS mass. The highest K is about 150 km s 1 for an MS star of initially 5 M fi. However, the sdB + NS systems that result from CE ejection have very short orbital periods and then high values of K (up to 800 km s 1). Such systems are born in very young populations (younger than 0.3 Gyr) and are potential gravitational wave sources that might be resolved by the Laser Interferometer Space Antenna (LISA) in the future. Gravitational wave radiation may again bring them into contact on a timescale of only similar to Myr. As a consequence, they are rare and hard to discover. The pulsar signal is likely a feature of sdB + NS systems caused by stable RLOF, and some NS components in sdB binaries may be millisecond pulsars. Various NS accretion efficiencies and NS masses change some properties of sdB + NS binaries, but not our general results.

Funding ProjectNatural Science Foundation of China[11733008] ; Natural Science Foundation of China[11422324] ; Natural Science Foundation of China[11521303] ; Natural Science Foundation of Yunnan province[2017HC018] ; Natural Science Foundation of Yunnan province[2013HA005]
Funding OrganizationNatural Science Foundation of China[11733008, 11422324, 11521303] ; Natural Science Foundation of Yunnan province[2017HC018, 2013HA005]
Language英语
Subject Area天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherEDP SCIENCES S A
Publication Place17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN1432-0746
URL查看原文
WOS IDWOS:000446426500002
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordWhite-dwarf Companions ; Electron-capture Supernovae ; Initial Mass Function ; O-type Subdwarf ; Millisecond Pulsars ; Hd 49798 ; Population Synthesis ; Driving Mechanism ; Radio Pulsars ; Kpd 1930+2752
EI Accession Number20184305970119
EI KeywordsWhite Dwarfs
EI Classification Number641.3mass Transfer - 657.2extraterrestrial Physics And Stellar Phenomena - 931.5gravitation, Relativity And String Theory - 941.3optical Instruments - 941.4optical Variables Measurements
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/18026
Collection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
Corresponding AuthorWu Y(吴优)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, PR China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, PR China
3.University of the Chinese Academy of Science, Beijing 100049, PR China
4.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, PR China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Wu Y,Chen XF,Li ZW,et al. Formation of hot subdwarf B stars with neutron star components[J]. ASTRONOMY & ASTROPHYSICS,2018,618:12.
APA Wu Y,Chen XF,Li ZW,&Han ZW.(2018).Formation of hot subdwarf B stars with neutron star components.ASTRONOMY & ASTROPHYSICS,618,12.
MLA Wu Y,et al."Formation of hot subdwarf B stars with neutron star components".ASTRONOMY & ASTROPHYSICS 618(2018):12.
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