The double helium-white dwarf channel for the formation of AM CVn binaries

作     者：Xian-Fei Zhang Jin-Zhong Liu C.Simon Jeffery Philip D.Hall Shao-Lan Bi 

作者机构：Department of AstronomyBeijing Normal University Xinjiang Astronomical ObservatoryChinese Academy of Sciences Armagh Observatory and PlanetariumCollege Hill School of PhysicsTrinity College Dublin 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2018年第18卷第1期

页      面：101-112页

核心收录：

学科分类：0709[理学-地质学] 07[理学] 0708[理学-地球物理学] 070401[理学-天体物理] 0825[工学-航空宇航科学与技术] 0704[理学-天文学] 

基　　金：supported by the CAS ‘Light of West China’ program(2015-XBQNA-02) the National Natural Science Foundation of China(NSFC,Grant Nos.10933002,11703001 and 11273007) the Joint Research Fund in Astronomy(U1631236) under cooperative agreement between the NSFC and the Chinese Academy of Sciences(CAS) the Strategic Priority Research Program of the Chinese Academy of Sciences(No.XDB2304100) the China Postdoctoral Science Foundation the Fundamental Research Funds for the Central Universities The Armagh Observatory and Planetarium are supported by a grant from the Northern Ireland Department for Communities support from the UK Science and Technology Facilities Council(STFC)(Grant No.ST/M000834/1) 

主　　题：stars:peculiar(helium) stars:white dwarfs binaries:close gravitational waves 

摘      要：Most close double helium white dwarfs will merge within a Hubble time due to orbital decay by gravitational wave ***,a significant fraction with low mass ratios will survive for a long time as a consequence of stable mass *** stable mass transfer between two helium white dwarfs（He WDs） provides one channel for the production of AM CVn binary *** previous calculations of double He WD progenitors,the accreting He WD was treated as a point *** have computed the evolution of 16 double He WD models in order to investigate the consequences of treating the evolution of both components in *** find that the boundary between binaries having stable and unstable mass transfer is slightly modified by this *** comparing with observed periods and mass ratios,we redetermine masses of eight known AM CVn stars by our double He WDs channel,*** Cnc,AM CVn,V406 Hya,J0926,J1240,GP Com,Gaia14 aae and V396 *** propose that central spikes in the triple-peaked emission spectra of J1240,GP Com and V396 Hya and the surface abundance ratios of N/C/O in GP Com can be explained by the stable double He WD *** mass estimates derived from our calculations are used to discuss the predicted gravitational wave signal in the context of the Laser Interferometer Space Antenna（LISA） project.