Very high energy radiation from binary system PSR B1259-63-SS 2883 [Elektronische Ressource] / presented by Hnatic Slavomir

Dissertationsubmitted to theCombined Faculties for the Natural Sciences and for Mathematicsof the Ruperto-Carola University of Heidelberg, Germanyfor the degree ofDoctor of Natural Sciencespresented byDiplom-Phys.: Hnatic Slavomirborn in: Sankt Petersburg, RussiaOral examination: 2 May 2007Very High Energy Radiation FromBinary System PSR B1259-63/SS 2883Referees: Prof. Dr. Stefan WagnerProf. Dr. Matthias BartelmanniAbstractThe inverse Compton (IC) scattering of ultrarelativistic electrons accelerated at the pulsar wind termi-nation shock is believed to be responsible for TeV gamma-ray signal reported from the binary system PSRB1259-63/SS2883. While this process can explain the energy spectrum of the observed TeV emission, thegamma-ray fluxes detected by HESS at different epochs do not agree with the published theoretical pre-dictions of the TeV lightcurve. In this work, evolution of the energy spectra of relativistic electrons underdifferent assumptions about the acceleration and energy-loss rates of electrons, is studied. Consequently, it isdemonstrated that the observed TeV lightcurve can be explained (i) by adiabatic losses which dominate overtheentire trajectory ofthepulsar with asignificant increase towards theperiastron, or (ii)bysub-TeVcutoffsin the energy spectra of electrons due to the enhanced rate of Compton losses close to the periastron.