TY  - JOUR
A1  - Meyer, Dominique M.-A.
A1  - Velazquez, Pablo F.
A1  - Petruk, Oleh
A1  - Chiotellis, Alexandros
A1  - Pohl, Martin
A1  - Camps-Farina, Artemi
A1  - Petrov, Miroslav
A1  - Reynoso, Estela M.
A1  - Toledo-Roy, Juan C.
A1  - Schneiter, E. Matias
A1  - Castellanos-Ramirez, Antonio
A1  - Esquivel, Alejandro
T1  - Rectangular core-collapse supernova remnants
BT  - application to Puppis A
JF  - Monthly notices of the Royal Astronomical Society
N2  - Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n approximate to 1 cm(-3), T approximate to 8000 K), an organized magnetic field of strength 7 mu G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M 0 star, that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A.
KW  - stars: evolution
KW  - stars: massive
KW  - ISM: supernova remnants
KW  - methods: MHD
Y1  - 2022
U6  - https://doi.org/10.1093/mnras/stac1832
SN  - 0035-8711
SN  - 1365-2966
VL  - 515
IS  - 1
SP  - 594
EP  - 605
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Meyer, Dominique M.-A.
A1  - Pohl, Martin
A1  - Petrov, Miroslav
A1  - Egberts, Kathrin
T1  - Mixing of materials in magnetized core-collapse supernova remnants
JF  - Monthly notices of the Royal Astronomical Society
N2  - Core-collapse supernova remnants are structures of the interstellar medium (ISM) left behind the explosive death of most massive stars ( ?40 M-?). Since they result in the expansion of the supernova shock wave into the gaseous environment shaped by the star's wind history, their morphology constitutes an insight into the past evolution of their progenitor star. Particularly, fast-mo ving massiv e stars can produce asymmetric core-collapse superno va remnants. We inv estigate the mixing of materials in core-collapse supernova remnants generated by a moving massive 35 M-? star, in a magnetized 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 organization of the supernova remnant and the more ef fecti ve the mixing of ejecta therein. In contrast, the mixing of stellar wind material is only weakly affected by progenitor motion, if at all.
KW  - ISM : supernova remnants
KW  - (magnetohydrodynamics) MHD
KW  - stars evolution
KW  - stars: massive
Y1  - 2023
U6  - https://doi.org/10.1093/mnras/stad906
SN  - 0035-8711
SN  - 1365-2966
VL  - 521
IS  - 4
SP  - 5354
EP  - 5371
PB  - Oxford Univ. Press
CY  - Oxford
ER  -