On the radial distribution of white dwarfs in the globular cluster NGC 6397

被引:32
作者
Davis, D. S. [1 ]
Richer, H. B. [1 ]
King, I. R. [2 ]
Anderson, J. [3 ]
Coffey, J. [1 ]
Fahlman, G. G. [4 ]
Hurley, J. [5 ]
Kalirai, J. S. [6 ]
机构
[1] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada
[2] Univ Washington, Dept Astron, Seattle, WA 98195 USA
[3] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA
[4] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada
[5] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia
[6] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA
关键词
stellar dynamics; stars : Population II; white dwarfs; globular clusters : individual : NGC 6397;
D O I
10.1111/j.1745-3933.2007.00402.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We have examined the radial distribution of white dwarfs over a single Hubble Space Telescope/Advanced Camera for Surveys field in the nearby globular cluster NGC 6397. In relaxed populations, such as in a globular cluster, stellar velocity dispersion, and hence radial distribution, is directly dependent on stellar masses. The progenitors of very young cluster white dwarfs had a mass of similar to 0.8 M-circle dot, while the white dwarfs themselves have a mass of similar to 0.5 M-circle dot. We thus expect young white dwarfs to have a concentrated radial distribution (like that of their progenitors) that becomes more extended over several relaxation times to mimic that of similar to 0.5M(circle dot) main-sequence stars. However, we observe young white dwarfs to have a significantly extended radial distribution compared both with the most massive main-sequence stars in the cluster and with old white dwarfs.
引用
收藏
页码:L20 / L24
页数:5
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