On the Formation of the Double Neutron Star Binary PSR J1846-0513  

作　　者：Long Jiang Kun Xu Shuai Zha Yun-Lang Guo Jian-Ping Yuan Xiang-Li Qian Wen-Cong Chen Na Wang 

机构地区：[1]School of Science,Qingdao University of Technology,Qingdao 266525,China [2]Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China [3]School of Physics and Electrical Information,Shangqiu Normal University,Shangqiu 476000,China [4]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [5]Department of Astronomy,Nanjing University,Nanjing 210023,China [6]Department of Intelligent Engineering,Shandong Management University,Jinan 250357,China

出　　处：《Research in Astronomy and Astrophysics》2024年第11期259-267,共9页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China(under grant Nos.12373044,12273014,12203051,12403035,12393811,12288102,and 12041304);the Natural Science Foundation of Shandong Province(under grant Nos.ZR2023MA050,and ZR2021MA013);the China Postdoctoral Science Foundation(under grant Nos.2024M751375 and 2024T170393);the Postdoctoral Fellowship Program of CPSF(under grant No.GZB20240307);the Jiangsu Funding Program for Excellent Postdoctoral Talent(under grant No.2024ZB705);the Tianshan Talent Program of Xinjiang Uygur autonomous region(under grant No.2023TSYCTD0013);the CAS“Light of West China”Program(under grant No.2018-XBQNXZ-B-022)。

摘　　要：The double neutron star PSR J1846-0513 is discovered by the Five-hundred-meter Aperture Spherical radio Telescope(FAST)in Commensal Radio Astronomy FAST Survey.The pulsar is revealed to be harbored in an eccentric orbit with e=0.208 and an orbital period of 0.613 day.The total mass of the system is constrained to b2.6287(35)M_(⊙),with a mass upper limit of 1.3455 M_(⊙)for the pulsar and a mass lower limit of 1.2845 M_(⊙)for th companion star.To reproduce its evolution history,we perform a 1D model for the formation of PSR J1846-0513whose progenitor is assumed to be neutron star—helium(He)star system via MESA code.Since the larg eccentricity is widely believed to originate from an asymmetric supernova explosion,we also investigate th dynamical effects of the supernova explosion.Our simulated results show that the progenitor of PSR J1846-0513could be a binary system consisting of a He star of 3.3-4.0 M_(⊙)and a neutron star in a circular orbit with an initia period of~0.5 day.

关 键 词：STARS evolution STARS NEUTRON (stars:)binaries general STARS individual(PSR J1864-0513) 

分 类 号：P145.6[天文地球—天体物理] P153[天文地球—天文学]