北京大学：《天文学》课程教学资源（PPT讲稿）Radio and Gamma-ray emission of pulsars

Radio and gamma-ray emission of pulsars Qiao, GJ Dept of Astronomy, Peking Univ Collaborators Zhang, B. University of Nevada, Xu,RX (PKU) Han,J. L NAOC), Lin, W.P. SHO),Lee, KJ(PKU) XiaXY

Qiao,G.J. Dept. of Astronomy, Peking Univ. Collaborators: Zhang, B.(University of Nevada), Xu, R.X.(PKU), Han,J.L.(NAOC), Lin,W.P.(SHO),Lee,K.J.(PKU) Xia,X.Y. Radio and Gamma-ray emission of pulsars

Radio and Gamma-ray emission of pulsars I Radio emission Inverse Compton scattering model: ICS II. Inner annular gap gamma-ray emission Radio t gamma ray emission III Pulsar: Neuron stars or Strange stars?

Radio and Gamma-ray emission of pulsars I. Radio emission (Inverse Compton scattering model: ICS ) II. Inner annular gap & gamma-ray emission Radio + Gamma ray emission III. Pulsar: Neuron stars or Strange stars?

Core beam Beam-frequency Bi-drifting Gamma-ray Mode changing Core gap Annular gap Strange stars

Core beam Beam-frequency Mode changing Bi-drifting Gamma-ray Core gap Annular gap Strange stars

Pulsar emission beams spin axis magnetic K to Earth Pulsar

Pulsar emission beams

Observations

Observations

Emission beams FIG. 21a Rankin,1983,Ap274,333

Emission beams Rankin, 1983, ApJ,274,333

Theories

Theories

Ruderman Sutherland(RS) Model FILLED CHARGE- SEPARATED MAGNE TOSPHERE E·B:0 GAP E.≠ STELLAR SURFACE E:0 Ruderman shutherland, 1975, ApJ, 196,51

Ruderman & Sutherland (RS) Model Ruderman & Shutherland,1975, ApJ,196,51

Emission beams in rs model FULSE EMVELOPE INTENSTY Emission beams AA∧ THE FIXED W LAST [+)OPEN FIELD LINE Hollow cone only! Ruderman sutherland. 1975

Emission beams in RS model Ruderman & Sutherland, 1975 Emission beams Hollow cone only!

Obs. Theory(cs) 1)Core+ Cones (2) Different components come from different locations (3) Pulse profile shapes changing with freq (4)Mode changing (5) Bi-drifting Pulsars: NS or Strange stars?

Obs. & Theory(ICS) (1) Core + Cones (2) Different components come from different locations (3) Pulse profile shapes changing with freq. (4) Mode changing (5) Bi-drifting  Pulsars: NS or Strange stars?