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Influence of the Secular Perturbation of an Intermediate-mass Companion. II. Ejection of Hypervelocity Stars from the Galactic Center
Zheng, Xiaochen1; Lin, Douglas N. C.2,3; Mao, Shude1,4
2021-06-01
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume914Issue:1Pages:13
AbstractThere is a population of stars with velocities in excess of 500 km s(-1) relative to the Galactic center. Many, perhaps most, of these hypervelocity stars (HVSs) are B stars similar to the disk and S stars in a nuclear cluster around a supermassive black hole (SMBH) near Sgr A(star). In Paper I of this series, we showed that the eccentricity of the stars emerged from a hypothetical disk around the SMBH that can be rapidly excited by the secular perturbation of its intermediate-mass companion (IMC), and we suggested IRS 13E as a potential candidate for the IMC. Here we show that this process leads to an influx of stars on parabolic orbits to the proximity of Sgr A(star) on a secular timescale of a few megayears. This timescale is much shorter than the diffusion timescale into the lost cone through either the classical or the resonant relaxation. Precession of the highly eccentric stars' longitude of periastron, relative to that of the IMC, brings them to its proximity within a few megayears. The IMC's gravitational perturbation scatters a fraction of the stars from nearly parabolic to hyperbolic orbits with respect to the SMBH. Their follow-up close encounters with the SMBH induce them to escape with hypervelocity. This scenario is a variant of the hypothesis proposed by Hills based on the anticipated breakup of some progenitor binary stars in the proximity of the SMBH, and its main objective is to account for the limited life span of the known HVSs. We generalize our previous numerical simulations of this process with a much wider range of orbital configurations. We demonstrate the robustness and evaluate the efficiency of this channel of HVS formation. From these numerical simulations, we infer observable kinematic properties for the HVSs.
Funding OrganizationNational Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation
DOI10.3847/1538-4357/abf5de
WOS KeywordBLACK-HOLE ; YOUNG STARS ; SPATIAL-DISTRIBUTION ; STELLAR DYNAMICS ; DENSITY PROFILE ; MILKY-WAY ; DISK ; BINARIES ; KINEMATICS ; GALAXY
Language英语
Funding ProjectNational Key Research and Development Program of China[2018YFA0404501] ; National Science Foundation of China[11821303] ; National Science Foundation of China[11761131004] ; National Science Foundation of China[11761141012] ; China Postdoctoral Science Foundation[2017M610865]
Funding OrganizationNational Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; China Postdoctoral Science Foundation ; China Postdoctoral Science Foundation
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000660969400001
PublisherIOP PUBLISHING LTD
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/77322
Collection中国科学院国家天文台
Corresponding AuthorZheng, Xiaochen
Affiliation1.Tsinghua Univ, Dept Astron, Beijing, Peoples R China
2.Univ Calif, Dept Astron & Astrophys, Santa Cruz, CA USA
3.Tsinghua Univ, Inst Adv Studies, Beijing, Peoples R China
4.Chinese Acad Sci, Natl Astron Observ China, 20A Datun Rd, Beijing, Peoples R China
Recommended Citation
GB/T 7714
Zheng, Xiaochen,Lin, Douglas N. C.,Mao, Shude. Influence of the Secular Perturbation of an Intermediate-mass Companion. II. Ejection of Hypervelocity Stars from the Galactic Center[J]. ASTROPHYSICAL JOURNAL,2021,914(1):13.
APA Zheng, Xiaochen,Lin, Douglas N. C.,&Mao, Shude.(2021).Influence of the Secular Perturbation of an Intermediate-mass Companion. II. Ejection of Hypervelocity Stars from the Galactic Center.ASTROPHYSICAL JOURNAL,914(1),13.
MLA Zheng, Xiaochen,et al."Influence of the Secular Perturbation of an Intermediate-mass Companion. II. Ejection of Hypervelocity Stars from the Galactic Center".ASTROPHYSICAL JOURNAL 914.1(2021):13.
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