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Markos Georganopoulos University of Maryland Baltimore County & NASA Goddard. Is the GeV emission of blazars really produced inside the broad line region?. External Compton scattering off the broad line ~10 eV photons. Sikora, Begelman, & Rees ‘94 >Spherical broad line region

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Markos Georganopoulos University of Maryland Baltimore County & NASA Goddard

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Markos GeorganopoulosUniversity of Maryland Baltimore County&NASA Goddard

Is the GeV emission of blazars really produced inside the broad line region?


External Compton scattering off the broad line ~10 eV photons

Sikora, Begelman, & Rees ‘94

>Spherical broad line region

with R~1017-18 cm

Uo UBLRΓ2

oBLRΓ 2 10 -4 in mc2 units


Kubo et al ‘98

Observed Compton dominance up to ~100 =>External Compton losses dominate

photons of ~ few GeV 

electrons of at least the same energy (γ~104)

For seed photons o~10-4

oγ~1

GeV emission comes from scatterings in the gray area between the Thomson and Klein-Nishina regimes


The devil is in the details…

At GeV electron energies the cooling time is

~ energy independent!

Effect on n(γ) ?


The devil is in the details…

At GeV electron energies the cooling time is

~ energy independent!

Effect on n(γ) ?


The electron distribution


How EC dominated blazars should look

  • Unavoidable but unobserved marks:

  • The hump in the synchrotron component

  • 2. The flat/rising SED of the GeV component (rarely seen, typical GeV spectrum is steep)

  • 3. Achromatic variability for the synchrotron hump and the GeV regime.


How EC dominated blazars should look

  • Unavoidable but unobserved marks:

  • The hump in the synchrotron component

  • 2. The flat/rising SED of the GeV component (rarely seen, typical GeV spectrum is steep)

  • 3. Achromatic variability for the synchrotron hump and the GeV regime.


Download the code at:

www.jca.umbc.edu/~markos/cs


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