| 書目名稱 | Neutron Stars 1 | | 副標題 | Equation of State an | | 編輯 | P. Haensel,A. Y. Potekhin,D. G. Yakovlev | | 視頻video | http://file.papertrans.cn/665/664683/664683.mp4 | | 叢書名稱 | Astrophysics and Space Science Library | | 圖書封面 |  | | 描述 | Neutron stars play a unique role in physics and astrophysics. On the one hand, they contain matter under extreme physical conditions, and their theories are based on risky and far extrapolations of what we consider reliable physical theories of the structure of matter tested in laboratory. On the other hand, their observationsoffertheuniqueopportunitytotestthesetheories. Moreover, n- tronstarsareimportantdramaticpersonaeonthestageofmodernastrophysics; they participate in many astronomical phenomena. ?3 Neutronstarscontainthematterofdensityrangingfromafew g cm attheir 15 ?3 surface, where the pressure is small, to more than 10 gcm at the center, 36 ?2 wherethepressureexceeds10 dyncm . Tocalculateneutronstarstructure, one needs the dependence of the pressure on density, the so called equation of state (EOS), in this huge density range, taking due account of temperature, 9 more than10 K in young neutron stars, and magnetic ?elds, sometimes above 15 10 G. The present book is mainly devoted to the theory of the EOS of neutron star matter and its consequences for neutron star structure. As one moves from the neutron star surface to the center, the methods to calculate the EOS change. Ato | | 出版日期 | Textbook 2007 | | 關(guān)鍵詞 | Star; Universe; book about neutron stars; dense matter; neutron star composition; neutron star magnetic f | | 版次 | 1 | | doi | https://doi.org/10.1007/978-0-387-47301-7 | | isbn_softcover | 978-1-4419-2214-4 | | isbn_ebook | 978-0-387-47301-7Series ISSN 0067-0057 Series E-ISSN 2214-7985 | | issn_series | 0067-0057 | | copyright | Springer-Verlag New York 2007 |
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