Flaring activity of microquasars from multi-frequency daily monitoring program with RATAN-600 radio telescope

Details Flaring activity of microquasars from multi-frequency daily monitoring program with RATAN-600 radio telescope Flaring activity of microquasars from multi-frequency daily monitoring program with RATAN-600 radio telescope

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..463t&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Computer Science

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Scientific paper

The powerful variable synchrotron emission is a tracer of the jet activity formation in the Galactic microquasars and in the extragalactic AGNs. During three last years we have carried out long monitoring programs of daily observations sets for microquasars with the RATAN radio telescope at 1-30 GHz. A lot of flaring events were detected when the fluxes increased by a factor of 2-200. The measured light curves are compared with the XTE ASM data to detect flaring activity correlations.
As a rule the powerful radio flares (SS433, Cyg X-3, LSI+61d303) were the optically thin, following a picture of the relativistic outflows from these compact X-ray binaries. Often flaring events in the active states (GRS1915+105, Cyg X-3, V4641 Sgr) show the inverted (optically thick) spectra with a spectral index >+1. We have detected clear X-ray/radio correlation (or association) in the light curves of GRS 1915+105 during October-November 2005, when it was very active (0.5-3 Crabs at 2-12 keV). As it was some times before, after 18 days of the quenched state (˜10 mJy) Cyg X-3 exhibited the 1Jy radio flare on 1 Feb 2006. It was also detected with Nobeyama 45m and NMA telescopes (Tsuboi et al. 2006, ATel #727), and in the first time a flat radio spectrum of the flaring event from Cyg X-3 was directly measured in the quasi-simultaneous observations from 2 to 110 GHz. Then two following flaring events (˜ 5 and ˜17 Jy) were detected later during ˜100 days. Their durations were ˜50 and ˜30 days respectively. The very fast rising flare, from 1 to 2 Jy during 3 hours, was detected with RT32 telescope (Trushkin et al. 2006, ATel #828) on 05 June. In our multi-frequency measurements we follow evolution of the powerful flares from a optically thick state to a optically thin one at lower frequencies, in coincidence with thermal absorption of the synchrotron radio emission from relativistic electrons bulky moved in the jets. We consider the temporal and spectral characteristics of the flares from microquasars using the finite segments jet model of the ejections.
This research is supported by Russian Foundation of Basic Research grant N 05-02-17556 and by the Program of the Praesidium of Russian Academy of Science.

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