Formation and Destiny of White Dwarf and Be Star Binaries  

作　　者：Chun-Hua Zhu Guo-Liang Lü Xi-Zhen Lu Jie He 

机构地区：[1]School of Physical Science and Technology,Xinjiang University,Urumqi 830046,China [2]Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China

出　　处：《Research in Astronomy and Astrophysics》2023年第2期262-274,共13页天文和天体物理学研究（英文版）

基　　金：the generous support of the Natural Science Foundation of Xinjiang No.2021D01C075;the National Natural Science Foundation of China;project Nos.12163005,U2031204 and 11863005;the science research grants from the China Manned Space Project with No.CMSCSST-2021-A10。

摘　　要：The binary systems consisting of a Be star and a white dwarf(Be WDs) are very interesting.They can originate from the binaries composed of a Be star and a subdwarf O or B star(Besd OBs),and they can merge into red giants via luminous red nova or can evolve into double WD potentially detected by the LISA mission.Using the method of population synthesis,we investigate the formation and the destiny of Be WDs,and discuss the effects of the metallicity(Z) and the common envelope evolution parameters.We find that Besd OBs are significant progenitors of Be WDs.About 30%(Z = 0.0001)-50%(Z = 0.02) of Be WDs come from Besd OBs.About 60%(Z = 0.0001)-70%(Z = 0.02) of Be WDs turn into red giants via a merger between a WD and a non-degenerated star.About 30%(Z = 0.0001)-40%(Z = 0.02) of Be WDs evolve into double WDs which are potential gravitational waves of the LISA mission at a frequency band between about 3 × 10^(-3)and 3 × 10^(-2)Hz.The common envelope evolution parameter introduces an uncertainty with a factor of about 1.3 on Be WD populations in our simulations.

关 键 词：(stars:)binaries(including multiple) close-stars evolution-stars rotation-(stars:)white dwarfs 

分 类 号：P145.5[天文地球—天体物理] P153[天文地球—天文学]