TY  - JOUR
AU  - Meyer, Dominique
AU  - Pohl, Martin
AU  - Petrov, M.
AU  - Egberts, K.
TI  - Mixing of materials in magnetized core-collapse supernova remnants
JO  - Monthly notices of the Royal Astronomical Society
VL  - 521
IS  - 4
SN  - 0035-8711
CY  - Oxford
PB  - Oxford Univ. Press
M1  - PUBDB-2023-06529
M1  - arXiv:2303.12579
SP  - 5354 - 5371
PY  - 2023
N1  - Accepted at MNRAS
AB  - Core-collapse supernova remnants are structures of the interstellar medium (ISM) left behind the explosive death of most massive stars (smaller or equal to 40 Mo). Since they result in the expansion of the supernova shock wave into the gaseous environment shaped by the star wind history, their morphology constitutes an insight into the past evolution of their progenitor star. Particularly, fast-moving massive stars can produce asymmetric core-collapse supernova remnants. We investigate the mixing of materials in core-collapse supernova remnants generated by a moving massive 35 Mo star, in a magnetised ISM. Stellar rotation and the wind magnetic field are time-dependently included into the models which follow the entire evolution of the stellar surroundings from the zero age main sequence to 80 kyr after the supernova explosion. It is found that very little main sequence material is present in remnants from moving stars, that the Wolf-Rayet wind mixes very efficiently within the 10 kyr after the explosion, while the red supergiant material is still unmixed by 30 per cent within 50 kyr after the supernova. Our results indicate that the faster the stellar motion, the more complex the internal organisation of the supernova remnant and the more effective the mixing of ejecta therein. In contrast, the mixing of stellar wind material is only weakly affected by progenitor motion, if at all.
LB  - PUB:(DE-HGF)16
UR  - <Go to ISI:>//WOS:000989560900020
DO  - DOI:10.1093/mnras/stad906
UR  - https://bib-pubdb1.desy.de/record/597256
ER  -