Qiao,G.J. Dept. of Astronomy, Peking Univ. Collaborators: Zhang, B.( University of Nevada ), Xu,...
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![Page 1: 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)](https://reader035.fdocuments.net/reader035/viewer/2022062423/56649ea15503460f94ba542b/html5/thumbnails/1.jpg)
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
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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?
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Core beamBeam-frequencyMode changing
Bi-drifting Gamma-ray
Core gap Annular gap
Strange stars
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Pulsar emission beams
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Observations
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Emission beams
Rankin, 1983, ApJ,274,333
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Theories
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Ruderman & Sutherland (RS) Model
Ruderman & Shutherland,1975, ApJ,196,51
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Emission beams in RS model
Ruderman & Sutherland, 1975
Emission beams
Hollow cone only!
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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?
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ICS Model: emission beams Core +cones⇒
Qiao, 1992
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ICS: shift of emission beams
Different emission location→shift ofthe emission beams
Qiao & Lin, 1998, A&A,333,172
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Poln: Beam shift→PA jumps
Xu, Qiao & Han, 1997, AA
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Poln: PA jump
Xu, Qiao & Han, 1997, AA
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ICS model: inner gap sparking →ω0
ω=2γ2ω0(1-βCosθi)
Qiao & Lin, 1998, A&A
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Core beamBeam-frequencyMode changing
Bi-drifting Gamma-ray
Core gap Annular gap
Strange stars
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RS model
Qiao,Liu, Zhang,& Han, 2001,AALyne & Manchester (1988) & Sieber et al. (1975),Kramer,(1994)
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“S” shape PA & Obs.
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Poln of integrated pulse in ICS
V—circular poln
L—Linear poln
I—Total Intensity
Position angle
Xu,Liu,Han,Qiao, 2000, ApJ
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Core beamBeam-frequencyMode changing
Bi-drifting Gamma-ray
Core gap Annular gap
Strange stars
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Mode changing of pulsars
Rankin, 1986
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Zhang,Qiao,Lin,Han, 1997
Tree mode of sparking
Thermal ICS
Curvature radiation
Resonant ICS
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Mode change pulsars
Zhang,Qiao,Lin,Han, 1997,ApJZhang,Qiao, Han, 1997,ApJ
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Core beamBeam-frequencyMode changing
Bi-drifting Gamma-ray
Core gap Annular gap
Strange stars
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☆ Polar cap (polar gap)
Basic Observational facts vs Theories
☆Radio--- Gamma-rays:
Obs.
Outer gapGamma-ray Radio
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The magnetosphere of a NS
+
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Inner annular gap
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Inner annular gap
Qiao,Lee,Wang,Xu, Han, 2004a,ApJL
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Inner annular gap
Qiao,Lee,Wang,Xu, 2004a, ApJL
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Inner Annular Gap
Qiao,Lee,Wang,Xu, 2004a, ApJL
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Core beamBeam-frequencyMode changing
Bi-drifting Gamma-ray
Core gap Annular gap
Strange stars
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Mclaughlin 2003,astr-ph/0310454
Bi-drifting: Obs.
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Drifting subpulses
PULSE LONGITUDE
Drifting subpulses
Taylor et al. (1975) Backer (1973)
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Accelerators:
• Inner vacuum gap (Ruderman & Sutherland 1975)
requiring high binding energy of charges on stellar surface
Drifting sub-pulses
Xu,Qiao Zhang,
1999,ApJL,522,L112
Deshpannde & Rankin,
1999,ApJ, 524,1008
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Inner Annular Gap : V= c E x B / B^2
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Bi-drifting: fitting
Mclaughlin 2003,astr-ph/0310454
Qiao,Lee,Zhang,Xu,Wang,2004b, ApJL
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Neutron stars:
Binding energy ≤ 10 KeV no gap can be formed!!! Binding energy > 10 KeV only one gap cab be formed: core or annular gap
Strange stars:
both core & annular gap can be Formed !
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● Annular Gap mole: different Gamma-ray pulsars can be fitted ● Pulsars: Strange stars?
● Observational check: Polarization at high energy bands ● Theory: two caps=two gap?
Conclusion and discussion
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Core beamBeam-frequencyMode changing
Bi-drifting Gamma-ray
Core flow Annular flow
Neutron stars
?
??
Qiao,Lee,Zhang,Wang & Xu,,2005,
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• Can free flow produce drifting pulses?
• If not, can we distinguish NS from SS?
♣ More drifting phenomena need to be obs.
♣ Sub-millisecond pulsar need to be found?
100 m telescope will be helpful for the research above!
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?
100m at EffelsbergNew Green Bank Telescope
Jodrell Bank KaShi,China ?
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Thank you !
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Multi-cones in the ICS model
Qiao,Wang,Wang,Xu, 2002,ChJAA
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Multi-frequency fitting of PSR J0437-4715
Qiao,Wang,Wang,Xu, 2002,ChJAA
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Magnetosphere of pulsars
Goldreich & Julian (1969)
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Charge density — ρGJ
(Goldreich & Julian 1969 )
]sin)/(1[
1
24 22
crc
BE
0
Bc
rE
0 BE
0 BE
GJ
GJ
0// E
0// E
Acceleration electric fieldAcceleration electric field
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Inner annular gap
Qiao,Lee,Wang,Xu, Han, 2004
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Ruderman & Sutherland, 1975
Neutron stars: binding energy > 10KeV
Can’t form core and annular gap at the same time!
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Strange stars: binding energy << 10KeV
Can form core and annular gap at the same time!
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Interstellar DispersionIonised gas in the interstellar medium causes lower radio frequencies to arrive at the Earth with a small delay compared to higher frequencies.
Given a model for the distribution of ionised gas in the Galaxy, the amount of delay can be used to estimate the distance to the pulsar.
P--period
DM--dispersion measure
msDMdt highlow 2261015.4
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Crab pulsar
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Vela Pulsar
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Geminga
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Inner annular gap
Qiao,Lee,Wang,Xu, 2003
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PAjumps: individual pulses ???
Stinebring et at. 1984
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OPM Depolarization (Xu.R.X)
Orthogonal Poln Mode (OPM) →Depolarization (Low LP] ???
Or
Low LP →OPM ???
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Daugherty &
Lerche, 1975
2
4.4 4exp( ), 1
/ 3q
e
Ble c m c B
The “Death line” of radio pulsars
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2
4.4 4exp( ), 1
/ 3q
e
Ble c m c B
h lB B B
1/ 24( / )
3Rc
2 22 (1 cos ) 2i mE
3.5 1.5 1ln ln
2AP P D P P
The Death line of radio pulsars
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Death and appearance line
Qiao et al.,2003
Sparking condition !
Does not Hubble line!
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The Death line of radio pulsars
Qiao & Zhang,1996
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The magnetosphere of a NS
Critical field line
NCS
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Low L Poln→OPM ?
Xu & Qiao, 2000, Science in China
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Outer Gap Model
Emission beams:
1 &4 : toward out side
2 & 3 : toward inside
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Muslimov & Harding, 2003
Slot gap model
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Beams in ICS model
Type I
Type II
Qiao,Liu,Zhang & Han, 2001
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Obs. & ICS : Type I a
Obs. ICS
Qiao,Liu, Zhang,& Han, 2001,AALyne & Manchester (1988) & Sieber et al. (1975)
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Obs. & ICS: Type Ib
Obs. ICS
Qiao,Liu, Zhang,& Han, 2001,AAKramer (1994).
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Obs. & ICS : Type IIa
ICS Obs.
Qiao,Liu, Zhang,& Han, 2001,AAPhillips & Wolszczan (1992).
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Magnetospere of pulsars
Am--mass of ion, Z-charge of ion
Outer gap, 1
Space charge limited flow
Inner gap
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Holloway 1975 MN
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Poln. of Individual pulses in ICS model
Xu,Liu,Han,Qiao, 2000, ApJ
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Radio emission of pulsars
Observations & Theories☆ Emission beams: Core+Cones Emission locations☆ Polarization: linear, circular, “orthogonal mode”☆ Pulse profiles changing with frequencies
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Rankin (1983, 1993)
Gil & Krawczyk 1996;Mitra & Deshpande 1999;
Gangadhara & Gupta 2001,
Lyne & Manchester 1988
Han & Manchester 2001
Core and Cones
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ω=2γ2ω0(1-βCosθi)
ICS model: The low frequency wave can Propagate near the surface
Qiao & Lin, 1998, AA
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Polar Cap Model
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Inner annular gap
Qiao,Lee,Wang,Xu, 2003
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Gamma-ray +radio emission
Radio + Gamma ray emission model ☆ Basic picture ☆ Pulse profiles fitting: radio + Gamma-rays
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Gamma-ray emission of pulsars
● Current models ☆ Polar cap model ☆ Outer gap model ● Radio + Gamma ray emission model ☆ Basic picture ☆ Pulse profiles fitting: radio + Gamma-rays
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• Pulsars are broad-band emitters (gamma-ray, X-ray, optical, radio)
• Pulsars must be particle accelerators
• Two preferred acceleration regions:
--- Polar cap region --- Outer gap region
Pulsar Gaps
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●
Gamma-ray OBS. Of Radio Pulsars
谢 谢 !
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Janssenet al. astr-ph/0406484: PSR B1818-13