Speaker
Description
First Name: Pablo
Last Name: Cerviño Solana
Affiliation: Universidad de Alcalá (UAH)
All Authors: Cerviño-Solana, Pablo; Blanco, Juan J.; Guerrero Contreras, Carlo Luis; Regadío, Alberto
Abstract: Charged particle acceleration within the solar atmosphere results from a complex combination of electromagnetic mechanisms that are not yet fully understood. A straightforward way to investigate this phenomenon is by analyzing its observable manifestation: the Solar Energetic Particles (SEPs) emitted from the Sun. Despite being the most common approach, it relies on the final outcome and thus fails to studying each mechanism independently. In addition, this approach only considers the outflow, neglecting a substantial fraction of the accelerated particles. Solar Neutrons (SNs) are produced in the inner layers of the solar atmosphere as a result of interactions between accelerated charged particles and the solar plasma. Since their production occurs in the photosphere, it is unaffected by processes in the outer corona, such as shock wave acceleration. Consequently, SN constitute an alternative approach to studying the effects of magnetic reconnection, one of the earliest particle acceleration mechanisms. Despite their potential, SNs have received little attention, especially regarding their production. In this work, we present a new tool for simulating both neutron production and escape in the solar photosphere. This tool has been developed using the particle transport and interaction simulation framework GEANT4.