On the Origin of Pulsar and Magnetar Magnetic Fields
arXiv:2111.01814 · doi:10.3847/1538-4357/ac4507
Abstract
In order to address the generation of neutron star magnetic fields, with particular focus on the dichotomy between magnetars and radio pulsars, we consider the properties of dynamos as inferred from other astrophysical systems. With sufficiently low (modified) Rossby number, convective dynamos are known to produce dipole-dominated fields whose strength scales with convective flux, and we argue that these expectations should apply to the convective proto-neutron stars at the centers of core-collapse supernovae. We analyze a suite of three-dimensional simulations of core collapse, featuring a realistic equation of state and full neutrino transport, in this context. All our progenitor models, ranging from 9 solar masses to 25 solar masses, including one with initial rotation, have sufficiently vigorous proto-neutron-star convection to generate dipole fields of order ~10^15 gauss, if the modified Rossby number resides in the critical range. Thus, the magnetar/radio pulsar dichotomy may arise naturally in part from the distribution of core rotation rates in massive stars.
arXiv commentAccepted for publication in ApJ; very minor changes from previous version
References in corpus (40)
- The ATNF Pulsar Catalogue
- Astrophysical magnetic fields and nonlinear dynamo theory
- Magnetars
- Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields
- Supernova Light Curves Powered by Young Magnetars
- The McGill Magnetar Catalog
- Birth and Evolution of Isolated Radio Pulsars
- Simulations of Magnetically-Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation
- A large scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae
- Three-dimensional core-collapse supernova simulated using a 15 progenitor
- The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations
- Three-Dimensional Simulations of Neutrino-Driven Core-Collapse Supernovae from Low-Mass Single and Binary Star Progenitors
- Self-consistent 3D Supernova Models From -7 Minutes to +7 Seconds: a 1-bethe Explosion of a ~19 Solar-mass Progenitor
- A Successful 3D Core-Collapse Supernova Explosion Model
- Modelling of isolated radio pulsars and magnetars on the fossil field hypothesis
- Ledoux-Convection in Protoneutron Stars --- a Clue to Supernova Nucleosynthesis?
- Fornax: a Flexible Code for Multiphysics Astrophysical Simulations
- Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M Stars
- Multi-Dimensional Radiation/Hydrodynamic Simulations of Protoneutron Star Convection
- High-Resolution Three-Dimensional Simulations of Core-Collapse Supernovae in Multiple Progenitors
- Magnetorotational core collapse of possible GRB progenitors. I. Explosion mechanisms
- Magnetar formation through a convective dynamo in protoneutron stars
- Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores
- Magnetorotational core collapse of possible GRB progenitors. III. Three-dimensional models
- A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations
- Turbulent Magnetic Field Amplification from Spiral SASI Modes: Implications for Core-Collapse Supernovae and Proto-Neutron Star Magnetization
- Asteroseismic signatures of evolving internal stellar magnetic fields
- Magnetorotational core collapse of possible GRB progenitors. II. Formation of protomagnetars and collapsars
- The Solar-Stellar Connection
- Magnetic Prandtl number dependence of kinetic to magnetic dissipation ratio
- Weak and Strong Field Dynamos: from the Earth to the stars
- Generation of Magnetic Fields by the Stationary Accretion Shock Instability
- Gravitational Waves from Neutrino Asymmetries in Core-Collapse Supernovae
- Long-term evolution of neutron-star merger remnants in general relativistic resistive-magnetohydrodynamics with a mean-field dynamo term
- A global model of the magnetorotational instability in protoneutron stars
- Neutrino viscosity and drag: impact on the magnetorotational instability in protoneutron stars
- Origin and evolution of magnetars
- Magnetized massive stars as magnetar progenitors
- Modelling spin evolution of magnetars
- General Relativistic Mean-field Dynamo Model for Proto-neutron Stars