Speaker
Description
Microquasars are primary candidates for Galactic PeVatrons, yet their collective contribution to the cosmic ray (CR) "knee" remains poorly understood. At PeV energies, local CR measurements are strongly influenced by individual Galactic PeVatrons and the Galactic magnetic field.
In this talk, we model the temporal and spatial distribution of source populations and transport Galactic CRs through the Galactic magnetic field. We show that the observed PeV proton "bump" can be naturally accounted for by a small number (≤ 4) of nearby microquasar remnants. Furthermore, we incorporate three-dimensional interstellar gas distributions for hadronic interactions and predict the diffuse fluxes of secondary neutrinos and gamma rays, showing good agreement with observations from IceCube and LHAASO. Finally, we discuss how different source populations shape the diffuse sky and highlight key implications for current and future multi-messenger observatories.
