PSR J2150+3427: A Possible Double Neutron Star System

Author:

Wu Q. D.,Wang N.ORCID,Yuan J. P.ORCID,Li D.ORCID,Wang P.ORCID,Xue M. Y.ORCID,Zhu W. W.ORCID,Miao C. C.ORCID,Yan W. M.ORCID,Wang J. B.ORCID,Yao J. M.ORCID,Wang S. Q.ORCID,Sun S. N.,Kou F. F.ORCID,Zhao D.ORCID,Chen Y. T.,Dang S. J.,Feng Y.ORCID,Liu Z. J.,Miao X. L.,Meng L. Q.ORCID,Yuan M.ORCID,Niu C. H.ORCID,Niu J. R.ORCID,Qian L.ORCID,Wang S.ORCID,Xie X. Y.,Xiao Y. F.,Yue Y. L.ORCID,You S. P.,Yu X. H.,Zhao R. S.,Yuen R.,Zhou X.ORCID,Zhang L.ORCID

Abstract

Abstract 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 ω ̇ = 0.0115(4) deg yr−1. An estimate for the total mass of the system using the ω ̇ 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 ω ̇ 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 ω ̇ , 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 E ̇ = 5.07(6) × 1029 erg s−1, PSR J2150+3427 is a very low-luminosity pulsar, with only the binary pulsar J2208+4610 having a smaller E ̇ .

Funder

The National Natural Science Foundation of China Grant

Publisher

American Astronomical Society

Subject

Space and Planetary Science,Astronomy and Astrophysics

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