An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311  

作　　者：LIU QingZhong1,2,LI Hui1,3 & YAN JingZhi1,2 1 Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China 2 Service d’Astrophysique,CEA Saclay and University Paris Diderot,91191 Gif-sur-Yvette,France 3 Graduate University of Chinese Academy of Sciences,Beijing 100049,China 

出　　处：《Science China(Physics,Mechanics & Astronomy)》2010年第S1期130-134,共5页中国科学：物理学、力学、天文学（英文版）

基　　金：supported by the National Basic Research Program of China (Grant No. 2009CB824800);the National High Technology Research and Development Program of China (Grant No. 2008AA12Z304);the National Natural Science Foundation of China (Grant Nos. 10873036 and 10673032)

摘　　要：The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated.Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet's diagram.The two SG/X-ray binaries,IGR J18483-0311 and OAO 1657-415,however,appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries.This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence.Here,we provide an alternative scenario to explain their location in Corbet's diagram:the SG/X-ray binaries are the descendants of Be/X-ray binaries,i.e.the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars.Furthermore,we suggest that there are two types of SG/X-ray binaries:one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history,and the other evolved from a Be/X-ray binary with an X-ray history.The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated.Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram.The two SG/X-ray binaries,IGR J18483-0311 and OAO 1657-415,however,appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries.This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence.Here,we provide an alternative scenario to explain their location in Corbet’s diagram:the SG/X-ray binaries are the descendants of Be/X-ray binaries,i.e.the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars.Furthermore,we suggest that there are two types of SG/X-ray binaries:one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history,and the other evolved from a Be/X-ray binary with an X-ray history.

关 键 词：high-mass X-ray BINARY pulsar Corbet’s DIAGRAM STELLAR EVOLUTION 

分 类 号：P144.9[天文地球—天体物理]