Roemer delay600Pulsar inecliptic400200(0-200Ecliptic latitude-400= 90 deg-6005000050500510005150052000525005300053500MJDCSIRO
Roemer delay Pulsar in ecliptic Ecliptic latitude = 90 deg
Details:Shapiro delayAt = Ac + AA + ABo + Aro + Aso - D/ f? + Avp + AB.Timedelaycausedbythepassageofthepulsethroughlargegravitational fields. Tempo2 includes delay caused by Sun (<110us),Jupiter(<180ns),Saturn(<58ns),Neptune(<12ns)andUranus (<10ns)0.000120.00018e-05(s)Keaodeus6e-054e-052e-050-2e-05500005050051000515005200052500530005350CMJDCSIRE
Details: Shapiro delay • Time delay caused by the passage of the pulse through large gravitational fields. Tempo2 includes delay caused by Sun (< 110us), Jupiter (<180ns), Saturn (<58ns), Neptune (<12ns) and Uranus (<10ns)
Details:dispersivedelayAt = Ac + AA + Aeo + Aro + Aso - D/f? + Avp + AB·D.is thedispersion constant.DM (cm-3pc)=2.410x10-16D·fisthefrequencyoftheradiationattheSolar Systembarycentre3.5e-053e-052.5e-05s)aoeos2e-051.5e-051e-055e-0605000050500510005150052000525005300053500MJD
Details: dispersive delay • D is the dispersion constant. DM (cm-3pc) = 2.410 x 10-16 D • f is the frequency of the radiation at the Solar System barycentre
Details:binary systemAt = Ac + AA + ABo + Aro + Aso - D/ f? + Avp + ABParameterDescriptionSymbolPBPbBinary period of pulsars (d)·ForpulsarsinbinaryECCeEccentricity of orbitAIXProjected semimajoraxis of orbit (lt-s)systems,tempo2includesTOToEpoch of periastron (MJD)OMLongitude of periastron (°)parametersdescribingtheTASCTacEpoch of ascending node (MJD)EPSIesinonorbital motion.EPS2Kecosw2KOMlongitude of the ascensing nodeKINiinclination angle.Various binary modelsSHAPMAXln (1 sina)3rexist. Suggest using"T2"aOMDOTPeriastron advance (deg yrl)A.PBDOTThe first time derivative of binary periodmodelthatcombinesmosteECCDOTRate of change ofeccentricity (s-l)AIDOTxRate of change of semimajor axis (lt-s'sl)GAMMAPost-Keplerian 'gamma' tem (s)YearlierbinarymodelsXPBDOTRate of change of orbital period minus GR prediction力EPSIDOTRate of change of EPS1REPS2DOTRate of change of EPS2MMTOTTotal system mass (Mo)M2Companion mass (Mo)m2DTHETARelativistic deformation of the orbitdoXOMDOTRate of periastron advance minus GR prediction (deg yr1)SINISine of inclination angle3DRdtRelativisticdeformation of the orbitAOAThe first aberration parameterBBOThe second aberration parameterBPB'Tensor multiscalar parameterBPPB"Tensormultiscalar parameterAFACAberrationgeometricfactorCSIRO
Details: binary system • For pulsars in binary systems, tempo2 includes parameters describing the orbital motion. • Various binary models exist. Suggest using “T2” model that combines most earlier binary models
Using the pulsar timing model·Havepulseemissiontimeinthepulsarframe·PredictusingthepulsartimingmodelReferencephasePulsefrequency(andtimederivatives)v(n-i)Ztpsrd(t) =+otpCn!n≥1PulseTime at whichemissiondo/dt= vtimePhaseofpulsesequence.Canalsoinclude simplemodel ofglitcheventsCSIR
Using the pulsar timing model • Have pulse emission time in the pulsar frame. • Predict using the pulsar timing model • Can also include simple model of glitch events Phase of pulse sequence Pulse frequency (and time derivatives) Pulse emission time Time at which df/dt = n Reference phase