The intensity and polarisation of the solar radio radiation over time in all available frequency channels is recorded.
For monitoring the solar activity and studies of the long-term evolution of solar active regions, images of the radio Sun will be taken with a cadence of 1/min. This is chosen to be in coincidence with the Global H alpha Network. The Sun will be observed at about 4 frequencies simultaneously, covering the whole LOFAR frequency range. Since the solar radio radiation is due to plasma emission, these frequencies correspond to different heights in the solar corona.
Joint observation campaigns of LOFAR with other ground-based and space-born instruments (e.g. GREGOR, ALMA, RHESSI, STEREO, Hinode and SDO) that observe the Sun in radio, optical, EUV, and X-ray wavelengths, enable dedicated studies of certain aspects of the solar activity, e.g. solar flares. Then, a higher image cadence of e.g. 0.1s is necessary in order to cover the dynamics of the burst.
For archiving the data of LOFAR's solar observations data a Solar Science Data Center is intended to establish for the whole LOFAR and solar physics community at the AIP. It can easily be extended to data form other experiments and to a general archive of solar data. Its organization is sketched below.