Formation of a Rapidly Rotating Classical Be-star in a Massive Close Binary System  

作　　者：Evgeny Staritsin 

机构地区：[1]K.A.Barkhatova Kourovka Astronomical Observatory,B.N.Yeltsin Ural Federal University,pr.Lenina 51,Ekaterinburg 620000,Russia

出　　处：《Research in Astronomy and Astrophysics》2024年第1期44-50,共7页天文和天体物理学研究（英文版）

基　　金：supported by the Ministry of Science and Education;FEUZ-2023-0019。

摘　　要：This paper investigates the spin-up of a mass-accreting star in a close binary system passing through the first stage of mass exchange in the Hertzsprung gap. Inside an accreting star, angular momentum is carried by meridional circulation and shear turbulence. The circulation carries part of the angular momentum of the accreted layers to the accretor's surface. The greater the rate of arrival of angular momentum in the accretor is, the greater this part. It is assumed that this part of the angular momentum can be removed by the disk further from the accretor. If the angular momentum in the matter entering the accretor is more than half the Keplerian value, then the angular momentum obtained by the accretor during mass exchange stage does not depend on the rate of arrival of angular momentum. The accretor may have the characteristics of a Be-star immediately after the end of mass exchange.

关 键 词：(stars:)binaries(including multiple):close stars:emission-line BE stars:early-type stars:rotation 

分 类 号：P153[天文地球—天文学]