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PSR J2150+3427: A Possible Double Neutron Star System

文献类型：期刊论文

作者Wu, Q. D.6,7,8,9; Wang, N.6,8,9; Yuan, J. P.6,8,9; Li, D.6,10,11; Wang, P.10,12; Xue, M. Y.10; Zhu, W. W.10,12; Miao, C. C.13; Yan, W. M.6,8,9; Wang, J. B.6,8,14
刊名ASTROPHYSICAL JOURNAL LETTERS
出版日期2023-11-01
卷号958期号:1页码:L17
ISSN号2041-8205
DOI10.3847/2041-8213/ad0887
产权排序1
英文摘要PSR J2150+3427 is a 0.654 s pulsar discovered by the Commensal Radio Astronomy FAST Survey. From the follow-up observations, we find that the pulsar is in a highly eccentric orbit (e = 0.601) with an orbital period of 10.592 days and a projected semimajor axis of 25.488 lt-s. Using 2.7 yr of timing data, we also measured the rate of periastron advance omega(center dot) = 0.0115(4) deg yr(-1). An estimate for the total mass of the system using the omega(center dot) gives M-tot = 2.59(13)M-circle dot, which is consistent with most of the known double neutron star (DNS) systems and one neutron star (NS)-white dwarf (WD) system named B2303+46. Combining omega(center dot) with the mass function of the system gives the masses of M-p < 1.67 and M-c > 0.98 M-circle dot for the pulsar and the companion star, respectively. This constraint, along with the spin period and orbital parameters, suggests that it is possibly a DNS system, and we cannot entirely rule out the possibility of an NS-WD system. Future timing observations will vastly improve the uncertainty in omega(center dot), and are likely to allow the detection of additional relativistic effects, which can be used to modify the values of M-p and M-c. With a spin-down luminosity of omega(center dot) = 5.07(6) x 10(29) erg s(-1), PSR J2150+3427 is a very low-luminosity pulsar, with only the binary pulsar J2208+4610 having a smaller omega(center dot).
WOS关键词RELATIVISTIC CELESTIAL MECHANICS ; PULSAR-TIMING PACKAGE ; RADIO PULSAR ; GENERAL-RELATIVITY ; BINARY-SYSTEMS ; DEATH LINE ; DISCOVERY ; LUMINOSITY ; TEMPO2 ; MODEL
资助项目This is work is supported by the National Key Research and Development Program of China (No. 2022YFC2205203), the National Natural Science Foundation of China grant (Nos. 12288102, 12041303, 12041304, 12273100, T2241020), and the Major Science and Technolo[2022YFC2205203] ; National Key Research and Development Program of China[U2031117] ; National Natural Science Foundation of China[2022A03013-2] ; National Natural Science Foundation of China[2022A03013-3] ; National Natural Science Foundation of China[2022A03013-4] ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region ; Xinjiang Uygur autonomous region of China[2021055] ; Youth Innovation Promotion Association CAS[YSBR-006] ; CAS Project for Young Scientists in Basic Reasearch[2020SKA0120200] ; National SKA Program of China[11873067] ; National Nature Science Foundation[ZK[2022]304] ; Guizhou Provincial Science and Technology Foundation[(2020) 003] ; Guizhou Provincial Science and Technology Foundation[2022D01D85] ; Foundation of Education Bureau of Guizhou Province, China ; Tianshan Talent project[YSBR-063] ; CAS Project for Young Scientists in Basic Research ; Chinese Academy of Sciences
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001108064500001
出版者IOP Publishing Ltd
资助机构This is work is supported by the National Key Research and Development Program of China (No. 2022YFC2205203), the National Natural Science Foundation of China grant (Nos. 12288102, 12041303, 12041304, 12273100, T2241020), and the Major Science and Technolo ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region ; Xinjiang Uygur autonomous region of China ; Youth Innovation Promotion Association CAS ; CAS Project for Young Scientists in Basic Reasearch ; National SKA Program of China ; National Nature Science Foundation ; Guizhou Provincial Science and Technology Foundation ; Foundation of Education Bureau of Guizhou Province, China ; Tianshan Talent project ; CAS Project for Young Scientists in Basic Research ; Chinese Academy of Sciences
源URL[http://ir.xao.ac.cn/handle/45760611-7/5616]  
专题脉冲星研究团组
新疆天文台_射电天文研究室
科研仪器设备产出_我台利用FAST观测数据文章
通讯作者Wang, N.; Yuan, J. P.; Li, D.
作者单位1.Cent China Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China
2.Guizhou Normal Univ, Guiyang 550001, Peoples R China
3.Xinjiang Univ, Dept Phys, Urumqi 830046, Peoples R China
4.Fudan Univ, Sch Comp Sci, Shanghai 200438, Peoples R China
5.GuiZhou Univ, Guiyang 550025, Guizhou, Peoples R China
6.Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1-St, Urumqi 830011, Xinjiang, Peoples R China
7.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
8.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Xinjiang, Peoples R China
9.Xinjiang Key Lab Radio Astrophys, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China
10.Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100101, Peoples R China
推荐引用方式
GB/T 7714		 Wu, Q. D.,Wang, N.,Yuan, J. P.,et al. PSR J2150+3427: A Possible Double Neutron Star System[J]. ASTROPHYSICAL JOURNAL LETTERS,2023,958(1):L17.
APA Wu, Q. D..,Wang, N..,Yuan, J. P..,Li, D..,Wang, P..,...&Zhang, L..(2023).PSR J2150+3427: A Possible Double Neutron Star System.ASTROPHYSICAL JOURNAL LETTERS,958(1),L17.
MLA Wu, Q. D.,et al."PSR J2150+3427: A Possible Double Neutron Star System".ASTROPHYSICAL JOURNAL LETTERS 958.1(2023):L17.

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