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Since its discovery more than hundred years ago, the origin of the cosmic-ray (CR) flux measured at Earth still remains unknown. To explain the energy region below the knee, located at few PeVs in the all-particle spectrum, supernova remnants (SNRs) are usually addressed as main CR accelerators. Nonetheless, experimental efforts searching for radiative signatures of PeV particles in SNR spectra could not yet probe their PeVatron capabilities, neither the hadronic origin of their emission. Recently, renewed interest was raised towards Young Massive Star Clusters (YMSCs) as an alternative candidate class of PeVatrons. In this contribution, I will discuss the physics of acceleration, propagation and radiation of high-energy particles in SNRs and YMSCs.
Silvia Celli got her PhD in early 2019 at Gran Sasso Science Institute (L’Aquila, Italy) under the supervision of Prof. Aharonian, exploring the physics of Galactic cosmic-ray accelerators with particular regards to supernova remnants. She then moved for a postdoc in Max Planck Institute for Nuclear Physics (Heidelberg, Germany), and later in Sapienza University (Rome, Italy) as L’Oreal-UNESCO fellow under the “Women in Science” project. She’s currently assistant professor at Sapienza University, working on synergy studies between gamma-ray and neutrino observatories.