The optical (BVRI) and radio (8.4 GHz) light curves of S5 1803+784 on a time span of nearly 6 yr are presented and discussed. The optical light curve showed an overall variation greater than 3 mag, and the largest changes occurred in three strong flares. No periodicity was found in the light curve on timescales up to a year. The variability in the radio band is very different and shows moderate oscillations around an average constant flux density rather than relevant flares, with a maximum amplitude of ~30%, without a simultaneous correspondence between optical and radio luminosity. The optical spectral energy distribution was always well fitted by a power law. The spectral index shows small variations, and there is indication of a positive correlation with the source luminosity. Possible explanations of the source behavior are discussed in the framework of current models.
Optical and radio monitoring of S5 1803+784
2002
Abstract
The optical (BVRI) and radio (8.4 GHz) light curves of S5 1803+784 on a time span of nearly 6 yr are presented and discussed. The optical light curve showed an overall variation greater than 3 mag, and the largest changes occurred in three strong flares. No periodicity was found in the light curve on timescales up to a year. The variability in the radio band is very different and shows moderate oscillations around an average constant flux density rather than relevant flares, with a maximum amplitude of ~30%, without a simultaneous correspondence between optical and radio luminosity. The optical spectral energy distribution was always well fitted by a power law. The spectral index shows small variations, and there is indication of a positive correlation with the source luminosity. Possible explanations of the source behavior are discussed in the framework of current models.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
