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Verfasst von:Pfrommer, Christoph [VerfasserIn]   i
 Pakmor, Rüdiger [VerfasserIn]   i
 Schaal, Kevin [VerfasserIn]   i
 Simpson, Christine M. [VerfasserIn]   i
 Springel, Volker [VerfasserIn]   i
Titel:Simulating cosmic ray physics on a moving mesh
Verf.angabe:C. Pfrommer, R. Pakmor, K. Schaal, C.M. Simpson and V. Springel
Jahr:2017
Jahr des Originals:2016
Umfang:30 S.
Fussnoten:Published online: 17 November 2016 ; Gesehen am 25.10.2017
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2017
Band/Heft Quelle:465(2017), 4, Seite 4500-4529
ISSN Quelle:1365-2966
Abstract:We discuss new methods to integrate the cosmic ray (CR) evolution equations coupled to magnetohydrodynamics on an unstructured moving mesh, as realized in the massively parallel arepo code for cosmological simulations. We account for diffusive shock acceleration of CRs at resolved shocks and at supernova remnants in the interstellar medium (ISM) and follow the advective CR transport within the magnetized plasma, as well as anisotropic diffusive transport of CRs along the local magnetic field. CR losses are included in terms of Coulomb and hadronic interactions with the thermal plasma. We demonstrate the accuracy of our formalism for CR acceleration at shocks through simulations of plane-parallel shock tubes that are compared to newly derived exact solutions of the Riemann shock-tube problem with CR acceleration. We find that the increased compressibility of the post-shock plasma due to the produced CRs decreases the shock speed. However, CR acceleration at spherically expanding blast waves does not significantly break the self-similarity of the Sedov-Taylor solution; the resulting modifications can be approximated by a suitably adjusted, but constant adiabatic index. In first applications of the new CR formalism to simulations of isolated galaxies and cosmic structure formation, we find that CRs add an important pressure component to the ISM that increases the vertical scaleheight of disc galaxies and thus reduces the star formation rate. Strong external structure formation shocks inject CRs into the gas, but the relative pressure of this component decreases towards halo centres as adiabatic compression favours the thermal over the CR pressure.
DOI:doi:10.1093/mnras/stw2941
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

kostenfrei: Volltext: http://dx.doi.org/10.1093/mnras/stw2941
 DOI: https://doi.org/10.1093/mnras/stw2941
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1564745864
Verknüpfungen:→ Zeitschrift

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