Rectangular core-collapse supernova remnants: Application to Puppis A

MEYER, D.M.-A.; VELÁZQUEZ, P.F.; PETRUK, O.; CHIOTELLIS, A.; POHL, M.; CAMPS-FARIÑA, A.; PETROV, M.; REYNOSO, E.M.; TOLEDO-ROY, J.C.; SCHNEITER, E.M.; CASTELLANOS-RAMÍREZ, A.; ESQUIVEL, A.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Año: 2022 vol. 515 p. 594 - 594

0035-8711

ore-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 ≈ 1 cm-3, T ≈ 8000 K), an organized magnetic field of strength 7μ 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⊙ 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 su