3D simulations of strongly magnetized non-rotating supernovae

• Verfasst von: Varma, Vishnu [VerfasserIn]
• Verfasst von: Müller, Bernhard [VerfasserIn]
• Verfasst von: Schneider, Fabian [VerfasserIn]
• Titel: 3D simulations of strongly magnetized non-rotating supernovae
• Titelzusatz: explosion dynamics and remnant properties
• Verf.angabe: Vishnu Varma, Bernhard Müller and Fabian R.N. Schneider
• E-Jahr: 2023
• Jahr: January 2023
• Umfang: 15 S.
• Fussnoten: Online verfügbar 11 November 2022 ; Gesehen am 30.01.2023
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2023
• Band/Heft Quelle: 518(2023), 3, Seite 3622-3636
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stac3247
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1832657965

Abstract

We investigate the impact of strong initial magnetic fields in core-collapse supernovae of non-rotating progenitors by simulating the collapse and explosion of a 16.9M⊙ star for a strong- and weak-field case assuming a twisted-torus field with initial central field strengths of ≈1012 and ≈106G⁠. The strong-field model has been set up with a view to the fossil-field scenario for magnetar formation and emulates a pre-collapse field configuration that may occur in massive stars formed by a merger. This model undergoes shock revival already 100ms after bounce and reaches an explosion energy of 9.3×1050erg at 310ms⁠, in contrast to a more delayed and less energetic explosion in the weak-field model. The strong magnetic fields help trigger a neutrino-driven explosion early on, which results in a rapid rise and saturation of the explosion energy. Dynamically, the strong initial field leads to a fast build-up of magnetic fields in the gain region to 40 per cent of kinetic equipartition and also creates sizable pre-shock ram pressure perturbations that are known to be conducive to asymmetric shock expansion. For the strong-field model, we find an extrapolated neutron star kick of ≈350kms−1⁠, a spin period of ≈70ms⁠, and no spin-kick alignment. The dipole field strength of the proto-neutron star is 2×1014G by the end of the simulation with a declining trend. Surprisingly, the surface dipole field in the weak-field model is stronger, which argues against a straightforward connection between pre-collapse fields and the birth magnetic fields of neutron stars.