Neutron Stars 1: Equation of State and StructureSpringer Science & Business Media, 2007 M12 6 - 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
3 | |
EQUILIBRIUM PLASMA PROPERTIES OUTER ENVELOPES 53 | 52 |
SkM interactions | 145 |
neutron matter | 152 |
ENVELOPES WITH STRONG MAGNETIC FIELDS | 166 |
netic field strength | 202 |
NUCLEONS AND HYPERONS 207 | 206 |
tribute to the NN interaction | 228 |
ANALYTICAL REPRESENTATIONS OF UNIFIED EOSs | 527 |
SEMIANALYTICAL EOSs IN NEUTRON STAR CORES | 533 |
111 | 536 |
BIBLIOGRAPHY | 543 |
339 | 551 |
118 | 553 |
558 | |
125 | 567 |
NEUTRON STAR STRUCTURE | 281 |
16 | 285 |
mass for the FPS and SLy EOSs | 303 |
tional mass at M Mmin for the FPS and SLy EOSs | 316 |
93 | 333 |
106 | 340 |
1 | 351 |
10 | 359 |
1 | 385 |
STRANGE MATTER AND STRANGE STARS 407 | 406 |
THEORY VERSUS OBSERVATIONS | 455 |
Appendices | 517 |
336 | 526 |
Otras ediciones - Ver todas
Neutron Stars 1: Equation of State and Structure P. Haensel,A.Y. Potekhin,D.G. Yakovlev Vista previa limitada - 2006 |
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 approximation Astron Astrophys atomic baryon number binding energy calculated Chapter compact component configurations Coulomb crystal curves dense matter dependence effects energy density EOSs equation equilibrium Fermi fraction frequency function gravitational hadronic Haensel hyperons increase inner crust kaon kaon condensation Landau magnetic field maximum mass measured meson Mmax momentum nebula neutrino neutron matter neutron star neutron star cores neutron star crust neutron star models non-rotating npeµ matter nuclear matter nuclei nucleon number density observations obtained optical orbital oscillations parameters particles phase transition Phys pion pion condensation plasma Potekhin potential pressure proton quantizing quantum quark matter quark stars radiation radio pulsars radius references therein relativistic rotating stable strange matter strange quark strange stars strong magnetic fields strongly superfluid supernova surface symmetry temperature theory thermal thermodynamic unstable velocity white dwarf X-ray binaries Zdunik