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@ARTICLE{Das:483537,
      author       = {Das, Samata and Brose, Robert and Pohl, Martin and Meyer,
                      Dominique M.-A. and Sushch, Iurii},
      title        = {{P}article acceleration, escape and non-thermal emission
                      from core-collapse supernovae inside non-identical
                      wind-blown bubbles},
      reportid     = {PUBDB-2022-05382, arXiv:2408.15839},
      year         = {2024},
      note         = {$A\&A,$ 689 (2024) A9},
      abstract     = {In the core-collapse scenario, the supernova remnants
                      evolve inside the complex wind-blown bubbles, structured by
                      massive progenitors during their lifetime. Therefore,
                      particle acceleration and the emissions from these SNRs can
                      carry the fingerprints of the evolutionary sequences of the
                      progenitor stars. We time-dependently investigate the impact
                      of the ambient environment of core-collapse SNRs on particle
                      spectra and the emissions. We use the RATPaC code to model
                      the particle acceleration at the SNRs with progenitors
                      having ZAMS masses of 20 Msol and 60 Msol. We have
                      constructed the pre-supernova circumstellar medium by
                      solving the hydrodynamic equations for the lifetime of the
                      progenitor stars. Then, the transport equation for cosmic
                      rays, and magnetic turbulence in test-particle approximation
                      along with the induction equation for the evolution of
                      large-scale magnetic field have been solved simultaneously
                      with the hydrodynamic equations for the expansion of SNRs
                      inside the pre-supernova CSM. The structure of the wind
                      bubbles along with the magnetic field and the scattering
                      turbulence regulate the spectra of accelerated particles for
                      both SNRs. For the 60 Msol progenitor the spectral index
                      reaches 2.4 even below 10 GeV during the propagation of the
                      SNR shock inside the hot shocked wind. In contrast, we have
                      not observed persistent soft spectra at earlier evolutionary
                      stages of the SNR with 20 Msol progenitor, for which the
                      spectral index becomes 2.2 only for a brief period. Later,
                      the spectra become soft above ~10 GeV for both SNRs, as weak
                      driving of turbulence permits the escape of high-energy
                      particles from the remnants. The emission morphology of the
                      SNRs strongly depends on the type of progenitors. For
                      instance, the radio morphology of the SNR with 20 Msol
                      progenitor is centre-filled at early stages whereas that for
                      the more massive progenitor is shell-like.},
      cin          = {$Z_THAT$},
      ddc          = {520},
      cid          = {$I:(DE-H253)Z_THAT-20210408$},
      pnm          = {613 - Matter and Radiation from the Universe (POF4-613) /
                      DFG project G:(GEPRIS)445052434 - SFB 1491: Das Wechselspiel
                      der kosmischen Materie - von der Quelle bis zum Signal
                      (445052434)},
      pid          = {G:(DE-HGF)POF4-613 / G:(GEPRIS)445052434},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)25},
      eprint       = {2408.15839},
      howpublished = {arXiv:2408.15839},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2408.15839;\%\%$},
      doi          = {10.3204/PUBDB-2022-05382},
      url          = {https://bib-pubdb1.desy.de/record/483537},
}