Complex Spectral Variability from Intensive Multi-wavelength Monitoring of Mrk421 in 1998

Details Complex Spectral Variability from Intensive Multi-wavelength Monitoring of Mrk421 in 1998 Complex Spectral Variability from Intensive Multi-wavelength Monitoring of Mrk421 in 1998

2000-08-31

arxiv.org/abs/astro-ph/0008505v1

Astrophys.J. 542 (2000) L105-L110

Astronomy and Astrophysics

Astrophysics

10 pages, 4 figures, accepted for publication in ApJ Letters

Scientific paper

10.1086/312929

We conducted a multi-frequency campaign for the TeV blazar Mrk~421 in 1998 April. The campaign started from a pronounced high amplitude flare recorded by SAX and Whipple; ASCA observation started three days later. In the X-ray data, we detected multiple flares, occuring on time scales of about one day. ASCA data clearly reveal spectral variability. The comparison of the data from ASCA, EUVE and RXTE indicates that the variability amplitudes in the low energy synchrotron component are larger at higher photon energies. In TeV Gamma-rays, large intra-day variations -- which were correlated with the X-ray flux -- were observed when results from three Cherenkov telescopes are combined. The RMS variability of TeV Gamma--rays was similar to that observed in hard X-rays, above 10 keV. The X-ray light curve reveals flares which are almost symmetric for most of cases, implying the dominant time scale is the light crossing time through the emitting region. The structure function analysis based on the continuous X-ray light curve of seven days indicates that the characteristic time scale is ~0.5 day. The analysis of ASCA light curves in various energy bands appears to show both soft (positive) and hard (negative) lags. These may not be real, as systematic effects could also produce these lags, which are all much smaller than an orbit. If the lags of both signs are real, these imply that the particle acceleration and X-ray cooling time scales are similar.

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