Neutron Stars 1: Equation of State and StructureSpringer Science & Business Media, 2006 M11 3 - 620 páginas 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. |
Contenido
EQUILIBRIUM PLASMA PROPERTIES OUTER ENVELOPES 53 | 52 |
corrections | 90 |
STRUCTURE AND EOS OF NEUTRON STAR CRUSTS | 115 |
inner crust | 129 |
ENVELOPES WITH STRONG MAGNETIC FIELDS | 167 |
NUCLEONS AND HYPERONS 207 | 206 |
NEUTRON STAR STRUCTURE | 281 |
NEUTRON STARS WITH EXOTIC CORES | 351 |
THEORY VERSUS OBSERVATIONS | 455 |
stars | 506 |
Appendices | 517 |
ANALYTICAL REPRESENTATIONS OF UNIFIED EOSs | 527 |
SEMIANALYTICAL EOSs IN NEUTRON STAR CORES | 533 |
BIBLIOGRAPHY | 543 |
LIST OF SYMBOLS 597 | 596 |
LIST OF ABBREVIATIONS | 605 |
STRANGE MATTER AND STRANGE STARS 407 | 406 |
Otras ediciones - Ver todas
Neutron Stars 1: Equation of State and Structure P. Haensel,A.Y. Potekhin,D.G. Yakovlev Vista previa limitada - 2007 |
Neutron Stars 1: Equation of State and Structure P. Haensel,A.Y. Potekhin,D.G. Yakovlev Sin vista previa disponible - 2010 |
Términos y frases comunes
accretion adiabatic index approximation Astron Astrophys atomic baryon number binding energy calculated Chapter compact component configurations Coulomb crystal curve dense matter dependence droplet effects emission energy density EOSs equation equilibrium Fermi fraction frequency function g cm gravitational hadronic Haensel Hartree-Fock hyperons increase inner crust ionized kaon kaon condensation Landau magnetic field many-body measured meson Mmax momentum neutrino neutron matter neutron star neutron star cores neutron star crust NN interaction non-rotating nuclear matter nuclei nucleon number density observations obtained orbital parameters particles phase transition Phys pion pion condensation plasma Potekhin pressure proton quantum quark matter quark stars radial radius references therein relativistic rotating spherical spin stable stellar strange matter strange quark strange stars strong magnetic fields superfluid surface symmetry temperature theory thermal thermodynamic unstable white dwarf X-ray binaries Zdunik