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Star-Planet Interaction (SPI) is a broad phenomenological term which encompasses a variety of physical effects relevant for the evolution of extra-solar planetary systems, in particular for those hosting giant gas planets in close orbits around their parent star. While theoretical expectations of SPI are abundant, observational signatures are still elusive with current instrumentation and adopted observing strategies. I will review the state of the art on the matter, and possible future developments that may help us for a better characterization of exoplanets and their abitability conditions.

I will talk about two new possibilities to analyse the observational data on non-thermal emission of cosmic rays accelerated in supernova remnants (SNRs). The first one is related to the polarization images of SNRs. In fact, the polarized radio emission has been mapped with great detail in several Galactic supernova remnants, but has not yet been exploited to the extent it deserves. We have developed a method to model maps of the Stokes parameters for shell-like SNRs during their Sedov evolution phase. The second result bases on the time-dependent particle acceleration and relates the temporal evolution of the radio spectral index of SNR in the aftermath of the explosion to the gamma-ray spectrum at later stages. As a test case, we apply our method to describe gamma-rays from IC443; as a proxy of the IC443 parent supernova we consider SN1987A.

It is debated whether the long and intense flares observed on the PMS stars in Orion involve single and very long magnetic channels or much flatter loop arcades. This question is important because the long flaring channels may be so long as to connect the star to the circumstellar disk. In this work a new method solves the question …. (suspence is left on purpose).