86 GHz polarimetry of OVV1633+382 after a major mm flare

Details 86 GHz polarimetry of OVV1633+382 after a major mm flare 86 GHz polarimetry of OVV1633+382 after a major mm flare

2005-01-03

arxiv.org/abs/astro-ph/0501014v1

Astronomy and Astrophysics

Astrophysics

4 pages. 5 figures. Proceedings of the 7th European VLBI Network Symposium held in Toledo, Spain on October 12-15, 2004. Edito

Scientific paper

The 18 mag QSO 1633+382 (4C38.41, z=1.807) showed a very pronounced outburst in 2001/2002. With a peak amplitude of more than 9 Jy at 90GHz, this flare was brighter than any known previous flare in this source (data available since 1980).During onset, the mm-flare was particulary fast, with an increase of more than 2 Jy at 230 GHz in less than 8 days. Since January 2002, the mm-flux of 1633+382 is decaying. During this decline, however, local flux variations with amplitudes of 1-3 Jy were seen, indicative of underlying and more rapid source activity on time scales of 1-2 months. After the main peak occurring in 2001.99, the 90 GHz flux showed secondary maxima at approximately half year intervals in 2002.3, 2002.7 and 2003.13. This kind of periodicity might be explained via the lighthouse model (Camenzind and Krockenberger 1992), which is based on the magnetic accelerator of Blanford and Payne (1982). At present the millimeter flux is nearly back to its quiescent level of 2-2.5 Jy, which the source had before the flare began. Our VLBA Polarimetry monitoring started June 2002 during the onset of the flare. At cm wavelength, the flare is only marginally detected which implies very high opacity of the source.

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