Research Group

*For the complete team see the relative websites

In the frame of single-dish radio monitoring of the solar atmosphere with INAF radiotelescopes we are developing and exploiting innovative single-dish radio imaging techniques at high-frequencies up to 100 GHz. Since 2018, we have been monitoring the solar atmosphere in the 18-26 GHz frequency range providing weekly images, in perspective covering the entire current solar cycle up to 100 GHz.

After a first test campaign aimed at defining and optimizing solar imaging requirements for the radio telescopes, the system is ready for systematic monitoring of the Sun to provide: (1) accurate measurement of the brightness temperature of the radio quiet Sun component, that has been poorly explored in the 20-26 GHz range to date, and representing a significant constraint for atmospheric models; (2) characterization of the flux density, spectral properties and long-term evolution of dynamical features (active regions, coronal holes, loop systems, streamers and the coronal plateau); (3) prediction of powerful flares through the detection of peculiar spectral variations in the active regions, as a valuable forecasting probe for the Space Weather hazard network (see https://sites.google.com/inaf.it/sundish for details).

New technological and scientific challenges are expected in the perspective of the new instrumentation available up to 100 GHz. In particular, a new solar imaging system at high frequency was recently approved as a permanent observatory in Antarctica (Solaris project: https://sites.google.com/inaf.it/solaris). It combines the implementation of dedicated and interchangeable high-frequency receivers on existing small single-dish radio telescope systems (2.6m class) available in our laboratories, on the Alps and in polar regions. Operations in Antarctica will offer unique observing conditions (very low sky opacity and long Solar exposures for nearly 20h/day) and unprecedented Solar monitoring in radio W-band (70-120 GHz). This opens for the continuous monitoring of the chromosphere and the identification and spectral analysis of Active Regions before, after and during the occurrence of Solar flares.

The Solaris observatory will be the only Solar facility offering continuous monitoring at 100 GHz, and it will be able to collect and disseminate data in synergy with the existing national and international network of Space Weather facilities.