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Neutron Stars 1: Equation of State and Structure: 326 (Astrophysics and Space Science Library, 326) - Softcover
Synopsis
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. Atomic structure and plasma theories are used for the surface stellar layers. Deeper layers of the neutron star crust require nuclear theory combined with plasma physics, both in very exotic density-temperature regimes. Finally, the neutron star core necessitates many-body theory of dense strongly interacting systems,togetherwiththephysicsofstronginteractionsofelementaryparticles.
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From the Back Cover
The book gives an extended review of theoretical and observational aspects of neutron star physics. With masses comparable to that of the Sun and radii of about ten kilometres, neutron stars are the densest stars in the Universe. This book describes all layers of neutron stars, from the surface to the core, with the emphasis on their structure and equation of state. Theories of dense matter are reviewed, and used to construct neutron star models. Hypothetical strange quark stars and possible exotic phases in neutron star cores are also discussed. Also covered are the effects of strong magnetic fields in neutron star envelopes and a comparison on neutron star models with observations.
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Neutron Stars 1: Equation of State and Structure (Astrophysics and Space Science Library, 326)
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Condition: New. Dieser Artikel ist ein Print on Demand Artikel und wird nach Ihrer Bestellung fuer Sie gedruckt. An extended review of theoretical and observational aspects of neutron star physicsDescribes all layers of neutron stars, from the surface to the core, with the emphasis on their structure and equation of stateTheories of dens. Seller Inventory # 4172742
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Neutron Stars 1
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ISBN 10: 1441922148
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Taschenbuch. Condition: Neu. This item is printed on demand - it takes 3-4 days longer - Neuware -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. Atomic structure and plasma theories are used for the surface stellar layers. Deeper layers of the neutron star crust require nuclear theory combined with plasma physics, both in very exotic density-temperature regimes. Finally, the neutron star core necessitates many-body theory of dense strongly interacting systems,togetherwiththephysicsofstronginteractionsofelementaryparticles. 644 pp. Englisch. Seller Inventory # 9781441922144
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Neutron Stars 1: Equation of State and Structure (Astrophysics and Space Science Library (326), Band 326) : Equation of State and Structure
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Taschenbuch. Condition: Sehr gut. Gebraucht - Sehr gut SG - leichte Beschädigungen oder Verschmutzungen, ungelesenes Mängelexemplar, gestempelt - The book gives an extended review of theoretical and observational aspects of neutron star physics. With masses comparable to that of the Sun and radii of about ten kilometres, neutron stars are the densest stars in the Universe. This book describes all layers of neutron stars, from the surface to the core, with the emphasis on their structure and equation of state. Theories of dense matter are reviewed, and used to construct neutron star models. Hypothetical strange quark stars and possible exotic phases in neutron star cores are also discussed. Also covered are the effects of strong magnetic fields in neutron star envelopes. Seller Inventory # INF1000546123
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Neutron Stars 1 : Equation of State and Structure
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Springer New York, Springer New York, 2010
ISBN 10: 1441922148
ISBN 13: 9781441922144
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Taschenbuch. Condition: Neu. Druck auf Anfrage Neuware - Printed after ordering - 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. Atomic structure and plasma theories are used for the surface stellar layers. Deeper layers of the neutron star crust require nuclear theory combined with plasma physics, both in very exotic density-temperature regimes. Finally, the neutron star core necessitates many-body theory of dense strongly interacting systems,togetherwiththephysicsofstronginteractionsofelementaryp articles. Seller Inventory # 9781441922144
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Neutron Stars 1
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Neutron Stars 1
Published by
Springer New York, Springer New York Nov 2010, 2010
ISBN 10: 1441922148
ISBN 13: 9781441922144
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Taschenbuch
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Taschenbuch. Condition: Neu. Neuware -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. Atomic structure and plasma theories are used for the surface stellar layers. Deeper layers of the neutron star crust require nuclear theory combined with plasma physics, both in very exotic density-temperature regimes. Finally, the neutron star core necessitates many-body theory of dense strongly interacting systems,togetherwiththephysicsofstronginteractionsofelementaryparticles.Springer Verlag GmbH, Tiergartenstr. 17, 69121 Heidelberg 644 pp. Englisch. Seller Inventory # 9781441922144
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Neutron Stars 1: Equation of State and Structure (Astrophysics and Space Science Library, 326)
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