Simulation of the orbit and spin period evolution of the double pulsars PSR J0737-3039 from their birth to coalescence induced by gravitational wave radiation  

作　　者：Peng Liu Yi-Yan Yang Jian-Wei Zhang Maria Rah 

机构地区：[1]School of Physics and Electronic Engineering,Qilu Normal University,Jinan 250200,China [2]School of Physics and Electronic Sciences,Guizhou Education University,Guiyang 550018,China [3]Astronomy Department,Beijing Normal University,Beijing 100875,China [4]Research Institute for Astronomy and Astrophysics of Maragha(RIAAM)-Maragha,Iran

出　　处：《Research in Astronomy and Astrophysics》2021年第4期319-324,共6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(NSFC,Grant Nos.11988101,11773005,U1631236,11703001,U1731238,U1938117,11725313,11721303);the International Partnership Program of Chinese Academy of Sciences(Grant No.114A11KYSB20160008);the National Key R&D Program of China(No.2016YFA0400702);supported by the National Basic Research Program(973 Program)(No.2015CB857100);National Key R&D Program of China(No.2017YFA0402600);the Guizhou Provincial Science and Technology Foundation(Grant No.[2020]1Y019)。

摘　　要：The complete orbital and spin period evolutions of the double neutron star(NS)system PSR J0737-3039 are simulated from birth to coalescence,which include the two observed radio pulsars classified as primary NS PSR J0737-3039 A and companion NS PSR J0737-3039 B.By employing the characteristic age of PSR J0737-3039 B to constrain the true age of the double pulsar system,the initial orbital period and initial binary separation are obtained as 2.89 h and 1.44 x 106 km,respectively,and the coalescence age or the lifetime from the birth to merger of PSR J0737-3039 is obtained to be 1.38×10^(8)yr.At the last minute of coalescence,corresponding to the gravitational wave frequency changing from 20 Hz to1180 Hz,we present the binary separation of PSR J0737-3039 to be from 442 km to 30 km,while the spin periods of PSR J0737-3039 A and PSR J0737-3039 B are 27.10 ms and 4.63 s,respectively.From the standard radio pulsar emission model,before the system merged,the primary NS could still be observed by a radio telescope,but the companion NS had crossed the death line in the pulsar magnetic-field versus period(B-P)diagram at which point it is usually considered to cease life as a pulsar.This is the first time that the whole life evolutionary simulation of the orbit and spin periods for a double NS system is presented,which provides useful information for observing a primary NS at the coalescence stage.

关 键 词：PSR J0737–3039 double neutron star pulsar gravitational wave SIMULATION 

分 类 号：P142[天文地球—天体物理]