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Titlebook: Structure and Evolution of Single and Binary Stars; C. W. H. Loore,C. Doom Book 1992 Springer Science+Business Media New York 1992 star.st

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发表于 2025-3-21 19:16:08 | 显示全部楼层 |阅读模式
书目名称Structure and Evolution of Single and Binary Stars
编辑C. W. H. Loore,C. Doom
视频videohttp://file.papertrans.cn/881/880190/880190.mp4
丛书名称Astrophysics and Space Science Library
图书封面Titlebook: Structure and Evolution of Single and Binary Stars;  C. W. H. Loore,C. Doom Book 1992 Springer Science+Business Media New York 1992 star.st
描述Classical stellar evolution theories have undergone somedrastic changes in recent decades. New insights into the developmentof stellar interiors were obtained from studying stars in variousstages of their lives, as well as with the help of fast computers,which gave a boost to the branch of numerical modelling of stellularstructure and evolution. .This book is divided into two parts. The first part deals with thegeneral aspects of stellular structure and evolution including achapter on numerical modelling. The second part deals with specificevolutionary aspects of single and binary stars with a variety ofmasses. The last chapter gives several models of stars with specificmasses. .The book is intended as an introduction for students, as well as areference for researchers.
出版日期Book 1992
关键词star; stars; stellar; stellar evolution; stellar structure
版次1
doihttps://doi.org/10.1007/978-94-011-2502-4
isbn_softcover978-0-7923-1844-6
isbn_ebook978-94-011-2502-4Series ISSN 0067-0057 Series E-ISSN 2214-7985
issn_series 0067-0057
copyrightSpringer Science+Business Media New York 1992
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Nuclear Reaction Rates,the star shine. These reactions transform lighter nuclei into heavier nuclei and produce energy as long as the binding energy per nucleon of the reacting particles is smaller than the binding energy per nucleon of the product of the reactions.
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Final Stages of Single Star Evolution, for a next burning phase if the temperature is high enough. The maximum temperature that can be attained in the stellar interior depends largely on the total mass of the star. It depends also on this temperature whether or not the produced ‘ashes’ will be ignited for a subsequent nuclear fusion phase.
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Structure and Evolution of Single and Binary Stars978-94-011-2502-4Series ISSN 0067-0057 Series E-ISSN 2214-7985
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