Extreme Physics andAstrophysics with Neutron Stars郑小平华中师范大学
Extreme Physics and Astrophysics with Neutron Stars 郑小平 华中师范大学
Configurationand ObservationsEOSofNuclearMatter.ViscositySomeMaximalAttributesofNeutronStars: Cooling.Remark
• Configuration and Observations • EOS of Nuclear Matter • Viscosity • Some Maximal Attributes of Neutron Stars • Cooling • Remark
TheoryObservationProblem:IEOSS of neutron stars is still an indeterminacyThe highly compressed mattershould transform into u,d,s quark mattertraditionalneutronstarquark-hybridstarNteN+e+nn.pe.uhyperon8Pneutronstarwithstarpioncondensaten.p,euudsquarksHyperons become populated2S0CE元inadditiontothenucleonscrustFecolor-superconducting36K10°gcmstrangequarkmatter(u,d,s quarks)11K10g'cm2SCCFL1014CSLgicmCFL-K+gCFLCFL-KLOFFHydrogen/HeCFL-元atmospherestrangestarnucleonstarIsospin symmetric nuclearStrange quark matter shouldR~10kmmatter-in equilibriumbemorestablethannuclearmatterwithcondensedK-meson
Problem: EOS of neutron stars is still an indeterminacy Theory Observation Isospin symmetric nuclear matter-in equilibrium with condensed K- meson Hyperons become populated in addition to the nucleons The highly compressed matter should transform into u,d,s quark matter Strange quark matter should be more stable than nuclear matter
Observational:masses(Msun)Taylor & Weisberg (1989):PSR1913+16 M-1.442+0.003 Most-robinariepreciseneutron-starmasses atbinarieswith95%confidencelevelompompRansom et al.(2005): M>1.68thecompdoubleDeutron starglobular cluster Terzan 5 at 95%mpbinariesHulse-Taylot pulsorconfidence levelinM15double putsarNice et al.(2005): PSRJ0751+1807 M=2.1+0.2neutronstar-whitedwarfbinarysystem3:48mspulsar业white dwart-Barret et al.(2005): LMXB 4Uneutron star2.95mspulsarbinariesn:47Tu1636-536 M-2.0+0.1HeutraegapbinaryCottam et al.(2002): EX0 0748-0.00.51.01.52.02.53.0Neutron star mass(Me)676 z-0.35Lattimeretal,astro-ph/0612440
Taylor & Weisberg (1989): PSR 1913+16 M=1.442+0.003 Most precise neutron-star masses at binaries with 95% confidence level Ransom et al.(2005): M>1.68 the globular cluster Terzan 5 at 95% confidence level Nice et al.(2005): PSR J0751+1807 M=2.1+0.2 a neutron star-white dwarf binary system Barret et al.(2005): LMXB 4U 1636-536 M=2.0+0.1 Cottam et al.(2002): EXO 0748- 676 z=0.35 Observational: masses(Msun) Lattimer et al, astro-ph/0612440
Observational: periods60Backer et al (1982)PSR B1937+21 1.58 mS(633 Hz) Natures40Fruchter et al (1988)PSR B1957+20 1.61 msJoai(621 Hz) NatureHessels et al(2006)20PSR J1748-2446ad1.39ms(719 Hz) ScienceKaaret et al(2007)XTE J1739-28500.110.0010.0110ars0.89ms(1122Hz)ApJLPulsar period (s)
Observational: periods Backer et al (1982) PSR B1937+21 1.58 ms (633 Hz) Nature Fruchter et al (1988) PSR B1957+20 1.61 ms (621 Hz) Nature Hessels et al(2006) PSR J1748-2446ad1.39 ms(719 Hz) Science Kaaret et al(2007) XTE J1739-285 0.89ms(1122Hz) ApJL