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| Home > Publications database > Particle acceleration, escape and non-thermal emission from core-collapse supernovae inside non-identical wind-blown bubbles |
| Journal Article | PUBDB-2022-07395 |
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2024
EDP Sciences
Les Ulis
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Please use a persistent id in citations: doi:10.1051/0004-6361/202245680 doi:10.3204/PUBDB-2022-07395
Report No.: arXiv:2408.15839
Abstract: Context. In the core-collapse scenario, the supernova remnants (SNRs) evolve inside the complex wind-blown bubbles,structured by massive progenitors during their lifetime. Therefore, particle acceleration and the emissions from theseSNRs can carry the fingerprints of the evolutionary sequences of the progenitor stars.Aims. We time-dependently investigate the impact of the ambient environment of core-collapse SNRs on particlespectra and the emissions, for two progenitors with different evolutionary tracks, accounting for the spatial transportof cosmic rays (CRs) and the magnetic turbulence which scatters CRs.Methods. We use RATPaC code to model the particle acceleration at the SNRs with progenitors having zero-age mainsequence (ZAMS) mass 20 M ⊙ , and 60 M ⊙ . We have constructed the pre-supernova circumstellar medium by solvingthe hydrodynamic equations for the lifetime of the progenitor stars. Then, the transport equation for cosmic rays, andmagnetic turbulence in test-particle approximation along with the induction equation for the evolution of large-scalemagnetic field have been solved simultaneously with the hydrodynamic equations for the expansion of SNRs inside thepre-supernova CSM in 1-D spherical symmetry.Results. The profiles of gas density and temperature of the wind bubbles along with the magnetic field and thescattering turbulence regulate the spectra of accelerated particles for both SNRs. The spectral index reaches 2.4 evenat lower energies (< 10 GeV) for 60 M ⊙ progenitor, during the propagation of SNR shock inside the shocked wind.However, we have not observed soft spectra persistently for the SNR with 20 M ⊙ progenitor at earlier evolutionarystages, where spectral index becomes 2.2 for a brief period during the interaction of SNR shock with the dense shellof red supergiant (RSG) wind material. At later stages of evolution, the spectra become soft above 1 GeV − 10 GeVfor both SNRs, as weakly driven turbulence, permits the escape of high-energy particles from the remnants. Further,the emission morphology of the SNRs strongly depend on the type of progenitors. For instance, radio morphology forthe SNR with 20 M ⊙ progenitor is centre-filled at early stages while, for the other one, the radio morphology is moreshell-like.
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