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@ARTICLE{Das:486640,
      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},
      journal      = {Astronomy and astrophysics},
      volume       = {689},
      issn         = {0004-6361},
      address      = {Les Ulis},
      publisher    = {EDP Sciences},
      reportid     = {PUBDB-2022-07395, arXiv:2408.15839},
      pages        = {A9},
      year         = {2024},
      note         = {$A\&A,$ 689 (2024) A9},
      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.},
      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)16},
      eprint       = {2408.15839},
      howpublished = {arXiv:2408.15839},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2408.15839;\%\%$},
      UT           = {WOS:001299482700010},
      doi          = {10.1051/0004-6361/202245680},
      url          = {https://bib-pubdb1.desy.de/record/486640},
}