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2024ApJ...964L...7Z - Astrophys. J., 964, L7 (2024/March-3)

A Relativistic Double Neutron Star Binary PSR J1846-0513.

ZHAO D., WANG N., YUAN J.P., LI D., WANG P., XUE M.Y., ZHU W.W., MIAO C.C., YAN W.M., WANG J.B., YAO J.M., WU Q.D., WANG S.Q., SUN S.N., KOU F.F., CHEN Y.T., DANG S.J., FENG Y., LIU Z.J., MIAO X.L., MENG L.Q., YUAN M., NIU C.H., NIU J.R., QIAN L., WANG S., XIE X.Y., XIAO Y.F., YUE Y.L., YOU S.P., YU X.H., ZHAO R.S., YUEN R., ZHOU X., ZHANG L., WANG Y.B., WU J.F., GAN Z.Y., SUN Z.Y. and WANG C.J.

Abstract (from CDS):

We report the timing analysis of PSR J1846-0513, a pulsar discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in Commensal Radio Astronomy FAST Survey. The pulsar possesses a spin period of 23.36 ms and a spin-down rate ($\dot{P}$) of 1.0106(3) × 10–18 s s–1, and it is located in an eccentric orbit (e ∼0.208) with an orbital period of 0.61 days. The characteristic age and surface magnetic field of the pulsar are found to be 366.62 Myr and 4.9178 × 109 G, respectively, indicating that it is a recycled pulsar. Using over two years of timing data, we measure the periastron advance $\dot{\omega }$ = 0.8956(8) deg yr–1. By assuming that this effect is purely relativistic, we have estimated the total mass M = 2.6287(35)M⊙ and obtained an upper limit for the pulsar mass and a lower limit for the companion's mass. Our results indicate that this is a double neutron star system.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Binary pulsars - Pulsars

Errata: erratum vol. 974, art. L39 (2024)

Simbad objects: 11

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