Variable accretion rates and fluffy first stars

被引:42
作者
Smith, Rowan J. [1 ]
Hosokawa, Takashi [2 ]
Omukai, Kazuyuki [3 ]
Glover, Simon C. O. [1 ]
Klessen, Ralf S. [1 ]
机构
[1] Univ Heidelberg, Zentrum Astron, ITA, D-69120 Heidelberg, Germany
[2] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA
[3] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan
基金
日本学术振兴会;
关键词
stars: formation; stars: Population III; stars: pre-main-sequence; early Universe; GAMMA-RAY BURSTS; INITIAL MASS FUNCTION; POPULATION III STARS; GRAVOTURBULENT FRAGMENTATION; TURBULENT FRAGMENTATION; PROTOSTELLAR FEEDBACK; EPISODIC ACCRETION; EVOLUTION; BINARIES; PROTOSTARS;
D O I
10.1111/j.1365-2966.2012.21211.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We combine the output of hydrodynamical simulations of Population III star cluster formation with stellar evolution models, and calculate the evolution of protostars experiencing variable mass accretion rates due to interactions within a massive disc. We find that the primordial protostars are extended fluffy objects for the bulk of their pre-main-sequence lifetimes. Accretion luminosity feedback from such objects is high, but, as shown in previous work, it has a minimal effect on the star cluster. The extended radii of the protostars, combined with the observation of close encounters in the simulations, suggest that mergers will occur in such systems. Furthermore, mass transfer between close protostellar binaries with extended radii could lead to massive tight binaries, which are a possible progenitor of gamma-ray bursts.
引用
收藏
页码:457 / 463
页数:7
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