Correction to: Spectrally resolved cosmic rays - II. momentum-dependent cosmic ray diffusion drives powerful galactic winds

• Verfasst von: Girichidis, Philipp [VerfasserIn]
• Verfasst von: Pfrommer, Christoph [VerfasserIn]
• Verfasst von: Pakmor, Rüdiger [VerfasserIn]
• Verfasst von: Springel, Volker [VerfasserIn]
• Titel: Correction to: Spectrally resolved cosmic rays - II. momentum-dependent cosmic ray diffusion drives powerful galactic winds
• Verf.angabe: Philipp Girichidis, Christoph Pfrommer, Rüdiger Pakmor and Volker Springel
• E-Jahr: 2023
• Jahr: 05 April 2023
• Umfang: 8 S.
• Fussnoten: Gesehen am 12.06.2023
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2023
• Band/Heft Quelle: 521(2023), 4 vom: Apr., Seite 5410-5417
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stad810
• Datenträger: Online-Ressource
• Sprache: eng
• Bibliogr. Hinweis: Ergänzung zu: Girichidis, Philipp: Spectrally resolved cosmic rays
• K10plus-PPN: 1848798806

Abstract

This erratum covers corrections to Girichidis et al. (2022). In the paper we present simulations with a new spectral cosmic ray (CR) solver, that includes energy dependent spatial diffusion and spectral cooling as introduced in Girichidis et al. (2020). We discuss one simulation with the new spectral solver (model ‘spectral’). Erroneously, the spectral cooling was not activated in the production run and the simulation effectively only included energy dependent diffusion and adiabatic gains and losses but no spectral CR cooling such as Coulomb and hadronic cooling. The originally identified dynamical differences between the grey CR models and the new spectral CRs are therefore significantly smaller. The different behaviour concerning the highest densities and the resulting star formation rate of the spectral model in Girichidis et al. (2022) must be attributed to the missing cooling rather than the spectral treatment of the CRs. Furthermore, the spectral shapes in the original paper are only altered by the energy dependent diffusion and not by the spectral cooling mechanisms. Several quantitative changes arise, but many qualitative differences between the grey and spectral models remain.