Synchrotron self-Compton flaring of TeV blazars. I. Linear electron cooling

Details Synchrotron self-Compton flaring of TeV blazars. I. Linear electron cooling Synchrotron self-Compton flaring of TeV blazars. I. Linear electron cooling

Jan 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...477..701s&link_type=abstract

Astronomy and Astrophysics, Volume 477, Issue 3, January III 2008, pp.701-715

Astronomy and Astrophysics

Astrophysics

4

Radiation Mechanisms: Non-Thermal, Galaxies: Active, Gamma Rays: Theory

Scientific paper

The vast improvement of the sensitivity of modern ground-based air Cherenkov telescopes, together with the sensitive flux measurements at lower frequencies, requires accurate elaborations of the theoretical radiation models for flaring blazars. Here the flaring of TeV blazars due to the synchrotron-self Compton (SSC) process is considered. We assume that, at the moment t=t_0, a flare in the emission knot occurs due to the instantaneous injection of monoenergetic (E_0) ultrarelativistic electrons. The ultrarelativistic electrons are injected uniformly over the knot volume and at later times are subject to linear synchrotron radiation cooling in a magnetic field whose strength remains constant during the time evolution of the relativistic electrons. The generated synchrotron photons are subject to multiple Thomson-scattering off the cold electrons in the source giving rise to spatial photon diffusion. Optically thick and thin synchrotron radiation intensities and photon density distributions in the emission knot as functions of frequency and time are analytically determined. The synchrotron photons serve as target photons for the SSC process, which is calculated in the optically thin frequency range using the Thomson approximation of the inverse Compton cross section. It is shown that the optically thick part of the synchrotron radiation process provides a negligible contribution to the resulting SSC intensity at all frequencies and times. Because the high-energy TeV photons undergo no elastic multiple Compton scatterings, we neglect the influence of photon diffusion in the calculation of the SSC intensity and fluence distribution with energy. The SSC fluence exhibits a break at E_f=15.8b-1/3 GeV from a ∝ E_s-1/4-power law spectrum at lower photon energies E_t≤ E_s≤ Ef to a ∝ E_s-2[1-(E_s/E_0)7/3]-distribution at high energies E_f≤ E_s≤ E_0. The application to the observed TeV fluence spectrum of the flare of PKS 2155-304 on July 28, 2006 yields δ b-1/3=27.1± 6.5. The emergent SSC light curve is independent of spatial photon diffusion and determined by the temporal variations on the relativistic electron density distribution and the synchrotron photon density. The comparison of the observed with the theoretical monochromatic synchrotron light curve determines the photon escape distribution.

Affiliated with

Also associated with

No associations

Rating

Synchrotron self-Compton flaring of TeV blazars. I. Linear electron cooling does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Synchrotron self-Compton flaring of TeV blazars. I. Linear electron cooling, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Synchrotron self-Compton flaring of TeV blazars. I. Linear electron cooling will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1587825