TY - JOUR
T1 - 3D simulations of strongly magnetized non-rotating supernovae
T2 - explosion dynamics and remnant properties
AU - Varma, Vishnu
AU - Müller, Bernhard
AU - Schneider, Fabian R.N.
N1 - Funding Information:
BM acknowledges support by ARC Future Fellowship FT160100035. This work is based on simulations performed within computer time allocations from Astronomy Australia Limited’s ASTAC scheme, the National Computational Merit Allocation Scheme (NCMAS), and an Australasian Leadership Computing Grant on the NCI NF supercomputer Gadi. This research was supported by resources provided by the Pawsey Supercomputing Centre, with funding from the Australian Government and the Government of Western Australia. This work has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 945806).
Publisher Copyright:
© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2023/1
Y1 - 2023/1
N2 - 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 16.9 M⊙ star for a strong- and weak-field case assuming a twisted-torus field with initial central field strengths of ≈1012 and ≈106 G. 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 100 ms after bounce and reaches an explosion energy of 9.3 × 1050 erg at 310 ms, 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 ≈350 km s−1, a spin period of ≈70 ms, and no spin-kick alignment. The dipole field strength of the proto-neutron star is 2 × 1014 G 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.
AB - 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 16.9 M⊙ star for a strong- and weak-field case assuming a twisted-torus field with initial central field strengths of ≈1012 and ≈106 G. 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 100 ms after bounce and reaches an explosion energy of 9.3 × 1050 erg at 310 ms, 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 ≈350 km s−1, a spin period of ≈70 ms, and no spin-kick alignment. The dipole field strength of the proto-neutron star is 2 × 1014 G 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.
KW - stars: magnetic fields
KW - stars: massive
KW - supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=85148367600&partnerID=8YFLogxK
U2 - 10.1093/mnras/stac3247
DO - 10.1093/mnras/stac3247
M3 - Article
AN - SCOPUS:85148367600
SN - 0035-8711
VL - 518
SP - 3622
EP - 3636
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -