X-RAY NETWORK FLARES OF THE QUIET SUN

Temporal variations in the soft X-ray (SXR) emission and the radio emi ssion above the solar magnetic network of the quiet corona are investi gated using Yohkoh SXR images with deep exposure and VLA observations in the centimeter radio range. The SXR data show several brightenings, with an extrapolated occurrence probability of one brightening per 3 seconds on the total solar surface. During the roughly 10 minutes of e nhanced flux, total radiative losses of the observed plasma are around 10(25) ergs per event. These events are more than an order of magnitu de smaller than previously reported X-ray bright points or active regi on transient brightenings. For all of the four SXR events with simulta neous radio observations, a corresponding radio source correlating in space and time can be found. There are several similarities between so lar flares and the SXR/radio events presented in this paper. (1) Varia tions in temperature and emission measure during the SXR enhancements are consistent with evaporation of cooler material from the transition region and the chromosphere. (2) The ratio of the total energies radi ated in SXR and radio frequencies is similar to that observed in flare s. (3) At least one radio event shows a degree of polarization as high as 35%. (4) In three out of four substructures the centimeter radio e mission peaks several tens of seconds earlier than in the SXR emission . (5) The associated radio emission tends to be more structured and to have faster rise times. These events thus appear to be flare-like and are called network flares.