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000597641 005__ 20240112093146.0
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000597641 0247_ $$2arXiv$$aarXiv:2303.12579
000597641 0247_ $$2datacite_doi$$a10.3204/PUBDB-2023-06636
000597641 037__ $$aPUBDB-2023-06636
000597641 041__ $$aEnglish
000597641 082__ $$a520
000597641 088__ $$2arXiv$$aarXiv:2303.12579
000597641 1001_ $$0P:(DE-H253)PIP1088512$$aMeyer, Dominique$$b0$$eCorresponding author
000597641 245__ $$aMixing of materials in magnetised core-collapse supernova remnants
000597641 260__ $$c2023
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000597641 3367_ $$2BibTeX$$aARTICLE
000597641 3367_ $$2DataCite$$aOutput Types/Working Paper
000597641 500__ $$aAccepted at MNRAS
000597641 520__ $$aCore-collapse supernova remnants are structures of the interstellar medium (ISM) left behind the explosive death of most massive stars (smaller or equal to 40 Mo). Since they result in the expansion of the supernova shock wave into the gaseous environment shaped by the star wind history, their morphology constitutes an insight into the past evolution of their progenitor star. Particularly, fast-moving massive stars can produce asymmetric core-collapse supernova remnants. We investigate the mixing of materials in core-collapse supernova remnants generated by a moving massive 35 Mo star, in a magnetised ISM. Stellar rotation and the wind magnetic field are time-dependently included into the models which follow the entire evolution of the stellar surroundings from the zero age main sequence to 80 kyr after the supernova explosion. It is found that very little main sequence material is present in remnants from moving stars, that the Wolf-Rayet wind mixes very efficiently within the 10 kyr after the explosion, while the red supergiant material is still unmixed by 30 per cent within 50 kyr after the supernova. Our results indicate that the faster the stellar motion, the more complex the internal organisation of the supernova remnant and the more effective the mixing of ejecta therein. In contrast, the mixing of stellar wind material is only weakly affected by progenitor motion, if at all.
000597641 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
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000597641 7001_ $$0P:(DE-H253)PIP1010085$$aPohl, Martin$$b1
000597641 7001_ $$0P:(DE-HGF)0$$aPetrov, Mihail$$b2
000597641 7001_ $$0P:(DE-H253)PIP1020748$$aEgberts, Kathrin$$b3
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000597641 9101_ $$0I:(DE-HGF)0$$6P:(DE-H253)PIP1088512$$aExternal Institute$$b0$$kExtern
000597641 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1010085$$aDeutsches Elektronen-Synchrotron$$b1$$kDESY
000597641 9101_ $$0I:(DE-HGF)0$$6P:(DE-H253)PIP1020748$$aExternal Institute$$b3$$kExtern
000597641 9131_ $$0G:(DE-HGF)POF4-613$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vMatter and Radiation from the Universe$$x0
000597641 9141_ $$y2023
000597641 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000597641 915__ $$0LIC:(DE-HGF)CCBY4$$2HGFVOC$$aCreative Commons Attribution CC BY 4.0
000597641 915__ $$0StatID:(DE-HGF)0580$$2StatID$$aPublished
000597641 9201_ $$0I:(DE-H253)Z_THAT-20210408$$kZ_THAT$$lTheoretische Astroteilchenphysik$$x0
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