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@ARTICLE{vanMarle:477572,
      author       = {van Marle, Allard Jan and Bohdan, Artem and Morris, Paul
                      and Pohl, Martin and Marcowith, Alexandre},
      title        = {{D}iffusive {S}hock {A}cceleration at {O}blique {H}igh
                      {M}ach {N}umber {S}hocks},
      journal      = {The astrophysical journal / 2},
      volume       = {929},
      number       = {1},
      issn         = {0004-637X},
      address      = {Chicago, Ill. [u.a.]},
      publisher    = {Univ.},
      reportid     = {PUBDB-2022-01938, arXiv:2203.00353. DESY-21-171},
      pages        = {7},
      year         = {2022},
      note         = {ISSN 1538-4357 not unique: **2 hits**.Accepted for
                      publication in ApJ},
      abstract     = {The current paradigm of cosmic-ray (CR) origin states that
                      the greater part of galactic CRs is produced by supernova
                      remnants. The interaction of supernova ejecta with the
                      interstellar medium after a supernova's explosions results
                      in shocks responsible for CR acceleration via diffusive
                      shock acceleration (DSA). We use particle-in-cell (PIC)
                      simulations and a combined PIC-magnetohydrodynamic (PIC-MHD)
                      technique to investigate whether DSA can occur in oblique
                      high Mach number shocks. Using the PIC method, we follow the
                      formation of the shock and determine the fraction of the
                      particles that gets involved in DSA. With this result, we
                      use PIC-MHD simulations to model the large-scale structure
                      of the plasma and the magnetic field surrounding the shock
                      and find out whether or not the reflected particles can
                      generate upstream turbulence and trigger DSA. We find that
                      the feasibility of this process in oblique shocks depends
                      strongly on the Alfvénic Mach number, and the DSA process
                      is more likely to be triggered at high Mach number shocks.},
      cin          = {$Z_THAT$},
      ddc          = {520},
      cid          = {$I:(DE-H253)Z_THAT-20210408$},
      pnm          = {611 - Fundamental Particles and Forces (POF4-611)},
      pid          = {G:(DE-HGF)POF4-611},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)16},
      eprint       = {2203.00353},
      howpublished = {arXiv:2203.00353},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2203.00353;\%\%$},
      UT           = {WOS:000780042800001},
      doi          = {10.3847/1538-4357/ac5962},
      url          = {https://bib-pubdb1.desy.de/record/477572},
}