Transport of Cosmic-Ray Electrons from 1 au to the Sun

Gamma rays are produced by cosmic ray (CR) protons interacting with the particles at solar photosphere and electrons positrons (CRes) via inverse Compton scattering of photons. The former come from disk while latter extend beyond disk. Evaluation these emissions requires flux spectrum CRs in vicinity Sun, most observations provide spectra near Earth, around 1 AU Sun. Past estimates quiet Sun gamma-ray emission use phenomenological modulation procedures to estimate (see review Orlando Strong 2021 references therein). We show that CRe transport inner heliosphere a kinetic approach novel approximation determine variation including effects (1) structure large scale magnetic field, (2) small turbulence wind several situ measurements, particular, those Parker Solar Probe this information 0.1 AU, (3) importantly, energy losses due synchrotron processes. present results on CRes for models. In forthcoming papers we will more accurate spectra, and, first time, extreme ultraviolet hard X-ray photons emission. These can be compared observation Fermi (see, e.g.~Fermi-LAT Collaboration, 2011) upper limits set RHESSI (Hannah et al., 2010).