Rectangular core-collapse supernova remnants: application to Puppis A

Abstract

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 ($n\approx 1\, \rm cm^{-3}$, $T\approx 8000\, \rm K$), an organised magnetic field of strength $7\, \mu \rm G$ has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper we show through 2.5D magneto-hydrodynamical simulations, in the context of a Wolf-Rayet-evolving $35\, \rm M_{\odot }$ star, that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age ($15\hbox{--}20\, \rm kyr$), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetised, 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.

Inside the core of a young massive star cluster: 3D MHD simulations

“…Some of the latest 3D HD/MHD models demonstrate the connection between the dynamical properties of SNRs and the internal structure of their progenitor stars, as well as the circumstellar medium (see Orlando et al 2020Orlando et al , 2022. Non-spherical morphology of SNRs propagating in anisotropic wind-blown bubbles shaped by interstellar magnetic fields has also been investigated by Meyer et al (2022). Recently, Meyer et al (2023) have studied the mixing of materials in magnetized core-collapse SNRs moving through the ISM over a period of ∼ 10 kyr.…”

The sculpting of rectangular and jet-like morphologies in supernova remnants by anisotropic equatorially confined progenitor stellar winds

“…Recently, Meyer et al (2022) studied the formation of SNRs with rectangular morphologies from a massive progenitor (35 M ). The remnant interacts with the stellar bubble resulting from the complex interaction of multiple subsequent wind phases: the O-type (main sequence) wind, the RSG phase, and finally a Wolf-Rayet (WR) wind.…”

“…By considering several azimuthal distributions of the stellar wind, we explore the final morphologies of the resulting SNRs and study whether such a scenario can reproduce and qualitatively explain the formation of SNRs with jet-like and rectangular morphologies. Unlike Meyer et al (2022), in this work, we will focus on studying SNRs from progenitors with stellar masses ≤ 16 M in the main sequence stage.…”