Confronting the neutron star population with inverse cascades
arXiv:2305.14347 · doi:10.3847/2041-8213/ace363
Abstract
The origin and evolution of magnetic fields of neutron stars from birth has long been a source of debate. Here, motivated by recent simulations of the Hall cascade with magnetic helicity, we invoke a model where the large-scale magnetic field of neutron stars grows as a product of small-scale turbulence through an inverse cascade. We apply this model to a simulated population of neutron stars at birth and show how this model can account for the evolution of such objects across the diagram, explaining both pulsar and magnetar observations. Under the assumption that small-scale turbulence is responsible for large-scale magnetic fields, we place a lower limit on the spherical harmonic degree of the energy-carrying magnetic eddies of . Our results favor the presence of a highly resistive pasta layer at the base of the neutron star crust. We further discuss the implications of this paradigm on direct observables, such as the nominal age and braking index of pulsars.
arXiv commentPublished in ApJL. 8 pages, 3 figures
References in corpus (27)
- The ATNF Pulsar Catalogue
- Birth and Evolution of Isolated Radio Pulsars
- Magnetic Field Evolution in Neutron Star Crusts due to the Hall Effect and Ohmic Decay
- Radio Pulsar Death Line Revisited: Is PSR J2144-3933 Anomalous?
- Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars
- A highly resistive layer within the crust of X-ray pulsars limits their spin periods
- Evolution of a buried magnetic field in the central compact object neutron stars
- New long-term braking index measurements for glitching pulsars using a glitch-template method
- Magnetic Fields from QCD Phase Transitions
- Radio efficiency of pulsars
- Hall drift and the braking indices of young pulsars
- psrqpy: a python interface for querying the ATNF pulsar catalogue
- Magnetic and Spin History of Very Young Pulsars
- Magnetic Axis Drift and Magnetic Spot Formation in Neutron Stars with Toroidal Fields
- MRI-driven dynamos in protoneutron stars
- Forward and inverse cascades in decaying two-dimensional electron magnetohydrodynamic turbulence
- A new scenario for magnetar formation: Tayler-Spruit dynamo in a proto-neutron star spun up by fallback
- Powering Central Compact Objects with a Tangled Crustal Magnetic Field
- Cascades in decaying three-dimensional electron magnetohydrodynamic turbulence
- MRI-driven dynamo at very high magnetic Prandtl numbers
- 3D Magneto-thermal Simulations of Tangled Crustal Magnetic Field in Central Compact Objects
- Hall cascade with fractional magnetic helicity in neutron star crusts
- 3D evolution of neutron star magnetic-fields from a realistic core-collapse turbulent topology
- Generating neutron-star magnetic fields: three dynamo phases
- Hosking integral in nonhelical Hall cascade
- Anisotropic electron transport in the nuclear pasta phase
- Exploring the neutron star zoo: An observational review