THE VELOCITIES OF INTRANETWORK AND NETWORK MAGNETIC-FIELDS

We analyzed two sequences of quiet-Sun magnetograms obtained on June 4 , 1992 and July 28, 1994. Both were observed during excellent seeing c onditions such that the weak intranet-work (IN) fields are observed cl early during the entire periods. Using the local correlation tracking technique, we derived the horizontal velocity fields of IN and network magnetic fields. They consist of two components: (1) radial divergenc e flows which move IN fields from the network interior to the boundari es, and (2) lateral flows which move along the network boundaries and converge toward stronger magnetic elements. Furthermore, we constructe d divergence maps based on horizonal velocities, which are a good repr esentation of the vertical velocities of supergranules. For the June 4 , 1992 data, the enhanced network area in the field of view has twice the flux density, 10% higher super granular velocity and 20% larger ce ll sizes than the quiet, unenhanced network area. Based on the number densities and flow velocities of IN fields derived in this paper and a previous paper (Wang et al., 1995), we estimate that the lower limit of total energy released from the recycling of IN fields is 1.2 x 10(2 8) erg s(-1), which is comparable to the energy required for coronal h eating.