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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2008年 / 383卷 / 01期

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

页码：L20 / L24

页数：5

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