Speaker
Description
The Sun in its quiescent state is a known gamma-ray source. The solar emission is produced by Cosmic Rays (CRs) penetrating the inner heliosphere and interacting with the solar atmosphere and optical photons. The solar emission is characterized by two spatially and spectrally distinct components: (i) the disk emission due to hadronic CR cascades in the solar atmosphere, and (ii) the spatially extended inverse Compton (IC) emission due to CR electrons scattering on the solar photons.
The intensity of both components anti-correlates with the solar activity being the brightest during solar minima. Observations of the two components at various solar activities allow to gain information on CRs very close to the Sun and on CR propagation in the heliosphere.
After the first observation of its gamma-ray emission in the EGRET archival data, Fermi-LAT is separating the two emission components with higher significance, allowing to precisely study the CR in the inner heliosphere.
We present updates of the models of the IC emission based on recent CR
measurements for various levels of solar activity, and we make predictions for e-ASTROGAM
and AMEGO, proposed low-energy gamma-ray missions.
