Particle acceleration and non-thermal radiation in young star clusters

Cosmic ray acceleration up to PeV energies has been suggested to take place in massive and young stellar clusters. The formation of a strong termination shock driven by the collective action of stellar winds in a compact cluster offers a promising location where efficient particle acceleration might take place. The subsequent hadronic collisions of these particles result into gamma-ray and neutrino production.

Within a scenario of particle acceleration at the cluster wind termination shock, we compute the expected gamma-ray and neutrino signals from both observed star clusters from the Gaia satellite as well as from the overall Galactic cluster population, evaluating detection prospects for both source and diffuse emissions from this source population by very-high-energy gamma-ray and neutrino instruments, as CTA, KM3NeT, and IceCube.

Fecha y lugar: 18/06/2026 – 12:30 | Salón de Actos
Silvia Celli
Sapienza University of Rome