致密双星 SS Cygni 的精确几何距离证实了吸积盘理论
高能天体物理现象
2013-05-28 v1
摘要
矮新星是从邻近红矮星伴星吸积物质的白矮星。它们的定期爆发由吸积盘中的热 - 粘滞不稳定性解释，这一机制由吸积盘不稳定性模型描述，该模型此后已成功扩展到其他吸积系统。然而，典型的矮新星 SS Cygni 对我们理解吸积盘理论提出了重大挑战。在哈勃空间望远镜测量的 159 +/- 12 pc 距离处，它过于明亮，无法发生观测到的定期爆发。利用甚长基线干涉测量 (VLBI) 射电观测，我们报告了 SS Cygni 的精确且与模型无关的距离，将该源定位在显著更近的 114 +/- 2 pc 处。这使得该源的行为与我们对吸积致密天体中吸积盘理论的理解相一致。
引用
@article{arxiv.1305.5846,
title = {An accurate geometric distance to the compact binary SS Cygni vindicates accretion disc theory},
author = {J. C. A. Miller-Jones and G. R. Sivakoff and C. Knigge and E. G. Körding and M. Templeton and E. O. Waagen},
journal= {arXiv preprint arXiv:1305.5846},
year = {2013}
}
备注
21 pages (8 as Supplementary Material), 3 figures (1 in the Supplementary Material). This is the authors' version of the work. It is posted here by permission of the AAAS for personal use, not for redistribution. The definitive version was published in Science in Vol. 340 no. 6135 on 24 May 2013