X-ray Spectral Variability of TeV Blazars during Rapid Flares

Details X-ray Spectral Variability of TeV Blazars during Rapid Flares X-ray Spectral Variability of TeV Blazars during Rapid Flares

2006-04-25

arxiv.org/abs/astro-ph/0604532v2

Astrophys.J.647:194-200,2006

Astronomy and Astrophysics

Astrophysics

17 pages, 4 figures, 4 tables, accepted by ApJ; one typo (unit of E_tot) corrected

Scientific paper

10.1086/505381

The spectral energy distribution (SED) of TeV blazars peaks both at keV and TeV energies. The X-ray emission is generally believed to originate in the synchrotron emission from relativistic electrons (and positrons) in the jet of these sources, while the origin of the gamma-ray emission is still being debated. We report results from a systematic study of X-ray spectral variability of Mrk 421 and Mrk 501 during individual flares that last for several days, making use of some of the high-quality data that have recently become available. The X-ray spectra of the two sources fall on the opposite sides of the synchrotron peak of their respective SEDs, so they together may offer additional insights into the physical origin of X-ray variability. We modeled each of the time-resolved X-ray spectra over a {\em single} flare by adopting a homogeneous spatial distribution and an instantaneous power-law spectral distribution for the emitting particles. We focused on the variation of four key parameters: particle spectral index, maximum Lorentz factor, energy density, and magnetic field. While there is considerable degeneracy in the fits, we show that, in order to account for the X-ray spectral variability observed in Mrk 421, at least three of the parameters are required to vary in most cases, with the spectral index being one of them. The observations of Mrk 501 support the conclusion, although the quality of the data is not as good. We discuss the implications of the results.

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