散射与距离关系[(s)0101001000DispersionmeasureDM (cm-3pc)Fig.21.16.The observed relation between pulse lengthening and dispersion measure.log1o t = -13.8 + 4.4log1o DM2013脉冲星暑期讲习班2013/8/216
10 10 log 13.8 4.4log = − + DM 散 射 与 距 离 关 系 2013/8/21 2013脉冲星暑期讲习班 6
散射导致脉冲轮廓展宽5msFig.21.15.Variable scattering in the Crab Nebula.Recordings at 408MHz of the interpulseoftheCrabpulsaroveraperiodofsixweeks(afterLyne&Thorne1975)2013/8/212013脉冲星暑期讲习班
散射导致脉冲轮廓展宽 2013/8/21 2013脉冲星暑期讲习班 7
星际磁场引起的法拉第旋转量RMddRM =neB//dl = 0.8131017.2元m2cl00(g_trpez)wavForMSPs,therearelittleornosignificant long-term variation inYanetal.2011,Ap&SSRMafterionosphericcorrectionJ160030537505002500250500750MJD54550SignificantRotationMeasurevariationsforVelapulsar(Hamilton(g.w pe)0etal.1985,MNRAS):measurea434A1970.01976.01979.01973.01982019850YEAR2013/8/2182013脉冲星暑期讲习班
星际磁场引起的法拉第旋转量RM Yan et al. 2011, Ap&SS • For MSPs, there are little or no significant long-term variation in RM after ionospheric correction. • Significant Rotation Measure variations for Vela pulsar (Hamilton et al. 1985, MNRAS): 2013/8/21 2013脉冲星暑期讲习班 8
星际闪烁Takenfrom"HandbookofPulsarAstronomy"byLorimer&Kramerandomlydistortedwavefrontsspatiallycoherentdiffractionradiationpattern00PSRPSRturbulentplasmaEarth(ISM)bulkeoadAnT.s4元2m2c经过薄屏后信号的相位和幅度的变化92013/8/212013脉冲星暑期讲习班
星际闪烁 经过薄屏后信号的相位和幅度的变化 2013/8/21 2013脉冲星暑期讲习班 9
星际闪烁081·展宽角径07a2元a8元ac·闪烁带宽4BB.82SSD'(An.)a4a:screensize薄屏模型可以较好地符合大部分观测现象102013/8/212013脉冲星暑期讲习班
星际闪烁 • 展宽角径 • 闪烁带宽 1 2 1 2 2 d e e D r n a = 2 d − 2 2 2 4 8 ( ) s e ac B D n 4 B s 薄屏模型可以较好地符合大部分观测现象 a: screen size 2013/8/21 2013脉冲星暑期讲习班 10