AAS 195th Meeting, January 2000
Session 98. Quasars and Their Cousins
Oral, Friday, January 14, 2000, 2:00-3:30pm, Centennial III

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[98.07] The origin of TeV gamma rays in blazars

K. K. Ghosh, B. D. Ramsey (NASA/MSFC, Space Science Department, SD50, Huntsville, AL35812), C. Sivaram (Indian Institute of Astrophysics, Bangalore 560 034, India)

TeV gamma ray emission has been detected from six blazars (3C66A, Mrk421, Mrk501, 1ES1959+658, PKS2155-304 and 1ES2344+514). Synchrotron, inverse-Compton, self- synchrotron inverse-Compton and proton cascade models have all been suggested for the production of TeV emission from these blazars. However these models have limitations in explaining the spectra of these objects in the X-ray through GeV band. Here we present the results of our model that is based on the physical processes in the shock-heated region in the relativistic jet. We suggest that the shock-heated region is produced by a blob which dumps its kinetic energy into the ambient medium of the jet. Then the shock-accelerated protons directly produce TeV gamma rays through interactions with the ambient protons. Subsequent cooling processes of the energetic electrons produce radio through GeV photons. The results of our computed model spectra fit well with the observed multifrequency (radio through TeV gamma rays) spectra of these six TeV blazars.

This work was performed while K. K. Ghsoh held a National Research Council (NASA/MSFC) Resident Research Associateship.

The author(s) of this abstract have provided an email address for comments about the abstract: kajal.ghosh@msfc.nasa.gov

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