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Introduction to the High Energy Astrophysics

Introduction to the High Energy Astrophysics. Introductory lecture. Cosmic Ray Spectrum ( nuclear component). 1 particle/m 2 s. Particle Flux ( m2 s sr GeV ) -1. „Knee ” 1 particle/m 2 yr. „Ankle ” 1 particle/km 2 yr. 1 J  6  10 18 eV. Energy eV. Zakres wysokich energii.

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Introduction to the High Energy Astrophysics

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  1. Introduction to the High EnergyAstrophysics Introductorylecture

  2. Cosmic Ray Spectrum (nuclear component) 1 particle/m2 s Particle Flux ( m2 s sr GeV )-1 „Knee” 1 particle/m2 yr „Ankle” 1 particle/km2 yr 1 J  61018 eV Energy eV

  3. Zakres wysokich energii E 2.5Particle Flux Energy (eV)

  4. SNR

  5. Black Holes

  6. Pulsary

  7. Crab Nebula : : wide frequency range electromagnetic spectrum - 20 decadesfotons – over 9 decades ! 100 keV – 100 TeV IC: syn, opt, IR, micro, CMB COMPTEL EGRET SYN HEGRA CELESTE B=160 G Ee ~1015 eV

  8. Quasars

  9. Takahashi et al. 2000 Mkn 421 SYN IC eV TeV keV TeV High variability: one looksinto vicinity of the central black hole czas w dniach

  10. Radiosources

  11. Solar magnetosphere

  12. B Stars Cosmic proton accelerators Dust Cosmic electron accelerators magnetic field adjusts relative height of peaks Radio Infrared Visible light X-rays VHE gamma rays SpectralEnergyDistribution: Energy emitted per log(E) interval f ~r

  13. Astronomicalosbervationcover a widerange of electromagneticwaves with characteristicfrequenciesorphotonenergies: 108 109 Hz – radio 1011 Hz – far IR 1014 Hz – close IR 1015 Hz – optical (eV) 1016 Hz – UV 1018 Hz – X-rays (keV) 1021 Hz – soft gamma rays (MeV) 1024 Hz – high energy gamma rays (GeV) 1027 Hz – very high energy gamma rays (TeV) 1029 Astronomyusesobservations of electromagneticsignals spanningover20 decades in frequency

  14. Observationalwindows of gamma rayastronomy: LE or MeV : 0.1 -100 MeV(0.1 -10+ 10 -100*) HE or GeV : 0.1 -100 GeV(0.1 -10 + 10 -100*) VHE or TeV : 0.1 -100 TeV(0.1 -10+ 10 -100*) UHE or PeV : 0.1 -100 PeV EHE or EeV : 0.1 -100 EeV are open in ranges of MeV, GeV, i TeV: LE,HE – observations from space VHE, .... -observations from the Earth surface * fewscientificresults

  15. Basicemissionprocesses with CR particles • Elektrons: • - Synchrotron emission („SYN”) • inmverse Compton emission („IC”) • nonthermal bremsstrahlung (usually not significant) • Protons: • - interactions p-p pions photons 

  16. Synchrotron emission("SYN") of relativisticelectronsspiraling in the magnetic field Emmittedenergy with maximum near (B-4  B/[10-4 G]) Dla B-4=1 i E~ GeV -> 108 Hz TeV -> 1014 Hz PeV -> 1020 Hz Hz Emissiontimescale lat for aboveB and E, respectively, ~106, ~103 i ~1 lat

  17. Inverse Compton emission("IC") of relativisticelectronsscatteringlowenergyphotons In the Thompson range( o  < mec2 , above: K-N) Emissiontimescale (with Uo,-10 = Uo/[10-10 erg/cm3]) lat Energies of scatteredphotons For example, for scattering of CMB photons(o~10-4 eV) and Ee = 1 GeV, 1 TeV, 1 PeV one receives' = 100 eV, 100 MeV, 100 TeV

  18. Cosmicobjects of interest for High EnergyAstrophysics neutron stars black holes NSXB BHXB accreting X-ray pulsars rotation powered pulsars milisecond pulsars plerions SNR cataclysmic variables microquasars Sgr A* stellar winds near O/B quasars balzars Syfert 1 Syfert 2 AGN MAS jets kpc-scale jets radio lobes hot spots in radio lobes GRB GRB afterglow soft gamma ray repeaters magnetars Solar protuberances interplanetary shock waves Earth magnetosphere CME cosmic rays high energy neutinos

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