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致密双星系统的演化

The Evolution of Compact Binary Star Systems.

作者信息

Postnov Konstantin A, Yungelson Lev R

机构信息

Sternberg Astronomical Institute, 13 Universitetskij Pr., 119992 Moscow, Russia.

Institute of Astronomy of Russian Academy of Sciences, 48 Pyatnitskaya Str., 119017 Moscow, Russia.

出版信息

Living Rev Relativ. 2006;9(1):6. doi: 10.12942/lrr-2006-6. Epub 2006 Dec 19.

DOI:10.12942/lrr-2006-6
PMID:28163653
原文链接:https://pmc.ncbi.nlm.nih.gov/articles/PMC5253975/
Abstract

We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Binary NSs and BHs are thought to be the primary astrophysical sources of gravitational waves (GWs) within the frequency band of ground-based detectors, while compact binaries of WDs are important sources of GWs at lower frequencies to be covered by space interferometers (LISA). Major uncertainties in the current understanding of properties of NSs and BHs most relevant to the GW studies are discussed, including the treatment of the natal kicks which compact stellar remnants acquire during the core collapse of massive stars and the common envelope phase of binary evolution. We discuss the coalescence rates of binary NSs and BHs and prospects for their detections, the formation and evolution of binary WDs and their observational manifestations. Special attention is given to AM CVn-stars - compact binaries in which the Roche lobe is filled by another WD or a low-mass partially degenerate helium-star, as these stars are thought to be the best LISA verification binary GW sources.

摘要

我们回顾了由白矮星（WDs）、中子星（NSs）和黑洞（BHs）组成的致密双星的形成与演化。双中子星和双黑洞被认为是地面探测器频段内引力波（GWs）的主要天体物理源，而白矮星致密双星则是空间干涉仪（LISA）将覆盖的较低频率引力波的重要源。讨论了当前对与引力波研究最相关的中子星和黑洞性质理解中的主要不确定性，包括致密恒星残骸在大质量恒星核心坍缩以及双星演化的共包层阶段所获得的初始速度的处理。我们讨论了双中子星和双黑洞的合并率及其探测前景、双白矮星的形成与演化及其观测表现。特别关注了类AM CVn星——一种致密双星，其洛希瓣被另一颗白矮星或低质量部分简并氦星充满，因为这些恒星被认为是LISA验证双星引力波源的最佳候选者。

https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/e6e5486dd563/41114_2016_6_Fig18.jpg
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https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/e6e5486dd563/41114_2016_6_Fig18.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/37cf428fc74c/41114_2016_6_Fig1.jpg
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https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/1665e796450f/41114_2016_6_Fig7.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/7c9f8838076a/41114_2016_6_Fig8.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/a11c45b0bd14/41114_2016_6_Fig9.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/b386b69b9602/41114_2016_6_Fig10.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/0941b503ea14/41114_2016_6_Fig11.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/e5715013ba6f/41114_2016_6_Fig12.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/cd93fadb51c4/41114_2016_6_Fig13.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/ded9d8f59f0a/41114_2016_6_Fig14.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/621abd48b064/41114_2016_6_Fig15.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/d24550ad0151/41114_2016_6_Fig16.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/389ad9e66f5f/41114_2016_6_Fig17.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/88af/5253975/e6e5486dd563/41114_2016_6_Fig18.jpg

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