PSR J2150+3427: A Possible Double Neutron Star System
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...
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| Format: | Article |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/ad0887 |
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| author | Q. D. Wu N. Wang J. P. Yuan D. Li P. Wang M. Y. Xue W. W. Zhu C. C. Miao W. M. Yan J. B. Wang J. M. Yao S. Q. Wang S. N. Sun F. F. Kou D. Zhao Y. T. Chen S. J. Dang Y. Feng Z. J. Liu X. L. Miao L. Q. Meng M. Yuan C. H. Niu J. R. Niu L. Qian S. Wang X. Y. Xie Y. F. Xiao Y. L. Yue S. P. You X. H. Yu R. S. Zhao R. Yuen X. Zhou L. Zhang |
| author_facet | Q. D. Wu N. Wang J. P. Yuan D. Li P. Wang M. Y. Xue W. W. Zhu C. C. Miao W. M. Yan J. B. Wang J. M. Yao S. Q. Wang S. N. Sun F. F. Kou D. Zhao Y. T. Chen S. J. Dang Y. Feng Z. J. Liu X. L. Miao L. Q. Meng M. Yuan C. H. Niu J. R. Niu L. Qian S. Wang X. Y. Xie Y. F. Xiao Y. L. Yue S. P. You X. H. Yu R. S. Zhao R. Yuen X. Zhou L. Zhang |
| author_sort | Q. D. Wu |
| collection | DOAJ |
| description | 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 $\dot{\omega }$ = 0.0115(4) deg yr ^−1 . An estimate for the total mass of the system using the $\dot{\omega }$ gives M _tot = 2.59(13) M _⊙ , 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 $\dot{\omega }$ with the mass function of the system gives the masses of M _p < 1.67 and M _c > 0.98 M _⊙ 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 $\dot{\omega }$ , 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 $\dot{E}$ = 5.07(6) × 10 ^29 erg s ^−1 , PSR J2150+3427 is a very low-luminosity pulsar, with only the binary pulsar J2208+4610 having a smaller $\dot{E}$ . |
| first_indexed | 2024-03-10T11:12:17Z |
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| id | doaj.art-768260cedc594d0c9cc8fea7c6df84af |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-10T11:12:17Z |
| publishDate | 2023-01-01 |
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| series | The Astrophysical Journal Letters |
| spelling | doaj.art-768260cedc594d0c9cc8fea7c6df84af2023-11-21T20:42:48ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019581L1710.3847/2041-8213/ad0887PSR J2150+3427: A Possible Double Neutron Star SystemQ. D. Wu0N. Wang1https://orcid.org/0000-0002-9786-8548J. P. Yuan2https://orcid.org/0000-0002-5381-6498D. Li3https://orcid.org/0000-0003-3010-7661P. Wang4https://orcid.org/0000-0002-3386-7159M. Y. Xue5https://orcid.org/0000-0001-8018-1830W. W. Zhu6https://orcid.org/0000-0001-5105-4058C. C. Miao7https://orcid.org/0000-0002-9441-2190W. M. Yan8https://orcid.org/0000-0002-7662-3875J. B. Wang9https://orcid.org/0000-0001-9782-1603J. M. Yao10https://orcid.org/0000-0002-4997-045XS. Q. Wang11https://orcid.org/0000-0003-4498-6070S. N. Sun12F. F. Kou13https://orcid.org/0000-0002-0069-831XD. Zhao14https://orcid.org/0009-0007-8062-1454Y. T. Chen15S. J. Dang16Y. Feng17https://orcid.org/0000-0002-0475-7479Z. J. Liu18X. L. Miao19L. Q. Meng20https://orcid.org/0000-0002-2885-568XM. Yuan21https://orcid.org/0000-0003-1874-0800C. H. Niu22https://orcid.org/0000-0001-6651-7799J. R. Niu23https://orcid.org/0000-0001-8065-4191L. Qian24https://orcid.org/0000-0003-0597-0957S. Wang25https://orcid.org/0000-0002-1570-7485X. Y. Xie26Y. F. Xiao27Y. L. Yue28https://orcid.org/0000-0003-4415-2148S. P. You29X. H. Yu30R. S. Zhao31R. Yuen32X. Zhou33https://orcid.org/0000-0003-4686-5977L. Zhang34https://orcid.org/0000-0001-8539-4237Xinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People's Republic of China; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; National Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of China; NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal , Durban 4000, South AfricaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of ChinaZhejiang Lab , Hangzhou, Zhejiang 311121, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Institute of Optoelectronic Technology, Lishui University , Lishui, 323000, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of China; Department of Physics, Xinjiang University , 830046, Urumqi, People's Republic of ChinaUniversity of Chinese Academy of Sciences , Beijing 100049, People's Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaGuizhou Normal University , Guiyang 550001, People's Republic of ChinaZhejiang Lab , Hangzhou, Zhejiang 311121, People's Republic of ChinaGuizhou Normal University , Guiyang 550001, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of China; Institute of Astrophysics, Central China Normal University , Wuhan 430079, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaSchool of Computer Science, Fudan University , Shanghai 200438, People's Republic of ChinaGuizhou Normal University , Guiyang 550001, People's Republic of ChinaGuiZhou University , Guizhou 550025, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaGuizhou Normal University , Guiyang 550001, People's Republic of ChinaGuizhou Normal University , Guiyang 550001, People's Republic of ChinaGuizhou Normal University , Guiyang 550001, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China ; na.wang@xao.ac.cn, yuanjp@xao.ac.cn, dili@nao.cas.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People's Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science1-Street, Urumqi, Xinjiang 830011, People's Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of ChinaPSR 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 $\dot{\omega }$ = 0.0115(4) deg yr ^−1 . An estimate for the total mass of the system using the $\dot{\omega }$ gives M _tot = 2.59(13) M _⊙ , 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 $\dot{\omega }$ with the mass function of the system gives the masses of M _p < 1.67 and M _c > 0.98 M _⊙ 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 $\dot{\omega }$ , 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 $\dot{E}$ = 5.07(6) × 10 ^29 erg s ^−1 , PSR J2150+3427 is a very low-luminosity pulsar, with only the binary pulsar J2208+4610 having a smaller $\dot{E}$ .https://doi.org/10.3847/2041-8213/ad0887Binary pulsarsPulsarsRadio pulsarsNeutron stars |
| spellingShingle | Q. D. Wu N. Wang J. P. Yuan D. Li P. Wang M. Y. Xue W. W. Zhu C. C. Miao W. M. Yan J. B. Wang J. M. Yao S. Q. Wang S. N. Sun F. F. Kou D. Zhao Y. T. Chen S. J. Dang Y. Feng Z. J. Liu X. L. Miao L. Q. Meng M. Yuan C. H. Niu J. R. Niu L. Qian S. Wang X. Y. Xie Y. F. Xiao Y. L. Yue S. P. You X. H. Yu R. S. Zhao R. Yuen X. Zhou L. Zhang PSR J2150+3427: A Possible Double Neutron Star System The Astrophysical Journal Letters Binary pulsars Pulsars Radio pulsars Neutron stars |
| title | PSR J2150+3427: A Possible Double Neutron Star System |
| title_full | PSR J2150+3427: A Possible Double Neutron Star System |
| title_fullStr | PSR J2150+3427: A Possible Double Neutron Star System |
| title_full_unstemmed | PSR J2150+3427: A Possible Double Neutron Star System |
| title_short | PSR J2150+3427: A Possible Double Neutron Star System |
| title_sort | psr j2150 3427 a possible double neutron star system |
| topic | Binary pulsars Pulsars Radio pulsars Neutron stars |
| url | https://doi.org/10.3847/2041-8213/ad0887 |
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