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Promieniowanie gamma pulsarów
i mgławic pulsarowych
Bronisław Rudak
CAMK
Przegorzały, 4-6.03.2013
Gwiazdy neutronowe
jako narzędzia fizyki i astrofizyki:
- poznanie równania stanu materii supergęstej
(neutrony + hiperony, kwarki, kondensaty mezonów)
- badanie propagacji fotonów w silnym polu magnetycznym
- badanie zjawisk relatywistycznej magnetohydrodynamiki
- testowanie teorii grawitacji w warunkach silnego pola grawitacyjnego
- testowanie modeli wybuchów supernowych
- detekcja fal grawitacyjnych pochodzenia kosmologicznego
+ ……….
Types of sources of interest in HE and VHE
domains
Rotation Powered Pulsars (RPP)
a) Classical pulsars
- young energetic (Crab, Vela)
- middle-aged (105 yr)
b) Millisecond pulsars (MSPs)
- individual MSPs
- ensembles of MSPs (in Globular Clusters)
c) RPP and their wind zones in massive binary systems
Magnetars
SGR and AXP
(cont.)
Pulsar Wind Nebulae
Physics of leptonic and hadronic pulsar winds powering their nebulae;
re-acceleration and diffusion of particles trapped in PWN.
Cosmic Ray Origin/SNRs/Mol.Clouds
Likely contribution of pulsars to the leptonic and hadronic components of CR.
5
Diagram of neutron star populations (Harding 2013)
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Why do pulsars radiateWhy do pulsars radiate
iinn the the high energyhigh energy domaindomain??
1) Rotating, strongly
magnetized neutron stars ->
unipolar inductors
2) Maximum potential drop (for vacuum rotator)
Vmax 6 1012 B12 P-2 Volts,
i.e. for young pulsars Vmax can exceed 1016 Volts.
Realistic potential drops are much smaller, but high enough
to accelerate charged particles to ultrarelativistic energies,
emitting in turn high energy photons.
Pulsar energy spectra and lightcurves
depend on
- location and spatial extent of accelerators,
- specific radiative processes,
- geometry (i.e. inclination and viewing angles)
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Radiative processes in Radiative processes in pulsar magnetospherespulsar magnetospheres
1. Curvature radiation
2. Inverse Compton Scattering (resonant + non-resonant)
3. Magnetic pair creation ( 1γ e± )
4. Photon-photon pair creation ( 2γ e± )
5. Synchrotron radiation
6. Photon splitting ( 1γ 2γ )
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3D TPC Slot Gap Model for the Crab Pulsar Harding, Stern, Dyks & Frackowiak 2008
= 45 deg
= 100 deg
CR + SR (primaries) + SR (pairs) + ICS (primaries with radio)
MAGIC
(inconsistent w. the MAGIC point)
The Crab Pulsar and 3D Outer Gap Model Hirotani, 2009
= 60 deg
= 113 deg
Synchro-curvature + ICS (pairs with IR)
Intrinsic: black line. Escaping: red line
MAGIC
11
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MAGIC Coll.+ Hirotani, 2011
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Abdo et al. 2009; Webb & Knoedlseder 2010
= 1.3 0.3
Ecutoff = 2.5 +1.6 -0.8 GeV
GlobularGlobular ClustersClusters withwith Fermi LATFermi LAT
((14 14 detecteddetected))
47 47 TucanaeTucanae TerzanTerzan 55 Kong et al. 2010
= 1.9 0.2
Ecutoff = 3.8 1.2GeV
HESS Collaboration, 2011
= 2.5 0.3
Discovery of VHE emission from the direction of Terzan 5
Zajczyk, Bednarek, R, 2013
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The online catalog TeVCat as of Nov 2011 (based on H.E.S.S., MAGIC, VERITAS)
Te
E > 0.1 TeV
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19 Aharonian, Bogovalov 2002
Pulsed
inside LC
Pulsed
outside LC
Unpulsed
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Spectral energy distribution of the Crab Nebula HE spectrum of the Crab pulsar
Super-flare on 2011 April 15-16
AGILE
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