Observational: thermal radiationJ.E.Truemper astro-ph/050245710aoBoond10°10°10101010Fé100ootaPlanckSpecdrum10ZKT=63Vpl10°Rm=4.4kma02dEnergy (keV)ndFig,J:The Chandra LETGX-ry spectrum of RX JI856 fitted with (non-magnetic)1photospheric models assuming pure iron and solar composition. The best fit is obtainedawithaPlanckspertrum(Burwitzetal.2003)
J. E. Truemper astro-ph/0502457 The magnetoshperic radiation Thermal emission from the polar caps Thermal emission from the bulk surface Observational: thermal radiation
Observational:: thermal radiationLo0tsdtkinStarlog10log10log10log10Kerg s-1yryr3.57+0.046.24+8843.90RXJ0822-424733.85-34.000.045.53+0.443.8586.21-881E1207.4-520933.27-33.74-0.193.96-806.03-833.08 -33.33RXJ0002+62464.26-85.83-884.0532.41-32.70PSR 0833-45 (Vela)5.8+0.134.24PSR 1706-4431.81-32.93-0.136.05-8184.47PSR 0538+281732.6-33.63.576.65-843.90RXJ0822-424733.60-33.905.53+0.443.85+0.486.48+0.011E1207.4-520932.70 -33.88=0.190.48-0.016.15+0.113.960RXJ0002+624632.18-32.81-0.116.18+0.024.26-8.174.0532.04-32.32PSR0833-45(Vela)-0.026.22+0.044.24PSR 1706-4432.48 -33.08-0.045.71±0.035.04PSR0656+1432.18-32.971-0.045.7595.53PSR 0633+174830.85-31.51一5.92+0.025.43PSR 1055-5232.07-33.192-0.025.70+0.055.6-5.9RXJ1856.5-375431.44-31.68-0.256.0±0.25.55-5.95RXJ0720.4-312531.3-32.5
Observational: thermal radiation
Observational:thermalradiationKargaltsev et al(2004)UV radiation, ApJ12.0-Io TT. Teur.-Stardb(kpc)T8(105K)p(ms)tsd(Myr)1395.761.24900PSRJ0437-47154.932707200< 4.6PSRJ2124-33584.873207700<9.2PSRJ0030+0451表5.2老年毫秒脉冲星旋转周期、年龄、距离与表面温度观测数据。引自文献[70]-14.030TFUV.110.12MK13km0.042MK14.5,37km111-15.015.015.516.016.517.017.518.0Log Frequency, Hz
Observational: thermal radiation Kargaltsev et al(2004) UV radiation, ApJ
Observational: thermal relaxationT-Treoe)onS1-01xg(_S shay mu toa#T-0T×gT-0T+r-01×S1-OTXr-O11-o1xg00T001OOT(1a)(A0)#品elPT880O50010001500050010001500Timesincet, (days)Timesincet。(days)KS 1731-260MXB1659-29
KS 1731 MXB 1659-29 -260 Observational: thermal relaxation
Compositioninside neutronstars?Classical:Compact stars (mainly)consist of neutronsExtended:Compact stars (mainly) consist of high density matter状态方程？超流？外壳输运？Veryhighdensity'afewoformorethan ten times the density of ordinaryatomicnucleiNeutronstarHighpressureenvironmentNumerous subatomicparticleprocessescompetewitheachother
Composition inside neutron stars? Neutron star Very high density:a few of or more than ten times the density of ordinary atomic nuclei High pressure environment Numerous subatomic particle processes compete with each other ? Classical: Compact stars (mainly) consist of neutrons Extended: Compact stars (mainly) consist of high density matter 状态方程？超流？外壳输运？