scholarly journals Magnetar formation through a convective dynamo in protoneutron stars

2020 ◽  
Vol 6 (11) ◽  
pp. eaay2732 ◽  
Author(s):  
Raphaël Raynaud ◽  
Jérôme Guilet ◽  
Hans-Thomas Janka ◽  
Thomas Gastine
Keyword(s):  
Gamma Ray ◽  
Magnetic Energy ◽  
Three Dimensional ◽  
Observational Constraints ◽  
Rotation Rates ◽  
Theoretical Support ◽  
Firm Basis ◽  
Protoneutron Stars ◽  
Protoneutron Star ◽  
Three Dimensional Simulations

The release of spin-down energy by a magnetar is a promising scenario to power several classes of extreme explosive transients. However, it lacks a firm basis because magnetar formation still represents a theoretical challenge. Using the first three-dimensional simulations of a convective dynamo based on a protoneutron star interior model, we demonstrate that the required dipolar magnetic field can be consistently generated for sufficiently fast rotation rates. The dynamo instability saturates in the magnetostrophic regime with the magnetic energy exceeding the kinetic energy by a factor of up to 10. Our results are compatible with the observational constraints on galactic magnetar field strength and provide strong theoretical support for millisecond protomagnetar models of gamma-ray burst and superluminous supernova central engines.

scholarly journals The impact of fallback on the compact remnants and chemical yields of core-collapse supernovae

2020 ◽  
Vol 495 (4) ◽  
pp. 3751-3762 ◽  
Author(s):  
Conrad Chan ◽  
Bernhard Müller ◽  
Alexander Heger
Keyword(s):  
Binding Energy ◽  
Gamma Ray ◽  
Three Dimensional ◽  
Explosion Energy ◽  
Core Collapse ◽  
Abundance Patterns ◽  
Small Set ◽  
The Impact ◽  
Disc Formation ◽  
Three Dimensional Simulations

ABSTRACT Fallback in core-collapse supernovae plays a crucial role in determining the properties of the compact remnants and of the ejecta composition. We perform three-dimensional simulations of mixing and fallback for selected non-rotating supernova models to study how explosion energy and asymmetries correlate with the remnant mass, remnant kick, and remnant spin. We find that the strongest kick and spin are imparted by partial fallback in an asymmetric explosion. Black hole (BH) kicks of several hundred $\mathrm{km}\, \mathrm{s}^{-1}$ and spin parameters of $\mathord {\sim }0.25$ can be obtained in this scenario. If the initial explosion energy barely exceeds the envelope binding energy, stronger fallback results, and the remnant kick and spin remain small. If the explosion energy is high with respect to the envelope binding energy, there is little fallback with a small effect on the remnant kick, but the spin-up by fallback can be substantial. For a non-rotating $12\, \mathrm{M}_\odot$ progenitor, we find that the neutron star is spun up to millisecond periods. The high specific angular momentum of the fallback material can also lead to disc formation around BHs. Fallback may thus be a pathway towards millisecond-magnetar or collapsar-type engines for hypernovae and gamma-ray bursts that does not require rapid progenitor rotation. Within our small set of simulations, none reproduced the peculiar layered fallback necessary to explain the metal-rich iron-poor composition of many carbon-enhanced metal-poor (CEMP) stars. Models with different explosion energy and different realizations of asymmetries may, however, be compatible with CEMP abundance patterns.

scholarly journals THREE-DIMENSIONAL SIMULATIONS OF LONG DURATION GAMMA-RAY BURST JETS: TIMESCALES FROM VARIABLE ENGINES

2016 ◽  
Vol 826 (2) ◽  
pp. 180 ◽  
Author(s):  
D. López-Cámara ◽  
Davide Lazzati ◽  
Brian J. Morsony
Keyword(s):  
Gamma Ray ◽  
Three Dimensional ◽  
Gamma Ray Burst ◽  
Long Duration ◽  
Three Dimensional Simulations

scholarly journals Three-dimensional simulations of magnetic reconnection in a dusty plasma

2008 ◽  
Vol 74 (4) ◽  
pp. 493-513 ◽  
Author(s):  
SAMUEL A. LAZERSON ◽  
HEINZ M. WIECHEN
Keyword(s):  
Magnetic Reconnection ◽  
Current Sheet ◽  
Dusty Plasma ◽  
Aerodynamic Drag ◽  
Magnetic Energy ◽  
Three Dimensional ◽  
Dust Particles ◽  
Classical Models ◽  
Parameter Dependent ◽  
Three Dimensional Simulations

AbstractWe present the results of three-dimensional self-consistent multi-fluid simulations of magnetic reconnection in a dusty plasma. We ballistically relax a Harris-like current sheet into a fluid pseudo-equilibrium. We then perturb the current sheet with typical inflow and outflow velocities associated with classical models of reconnection. We find a 20% decrease in magnetic energy for the case of a locally enhanced resistivity. For a parameter-dependent resistivity we find a 26% decrease in magnetic energy in the current sheet. We find dust-neutral relative flow velocities that are a factor of two greater than the dust Alfvén velocity. We then explore the implications of these flows on aerodynamic drag heating of the dust particles.

The wake behind a cylinder rolling on a wall at varying rotation rates

2010 ◽  
Vol 648 ◽  
pp. 225-256 ◽  
Author(s):  
B. E. STEWART ◽  
M. C. THOMPSON ◽  
T. LEWEKE ◽  
K. HOURIGAN
Keyword(s):  
Reynolds Number ◽  
Three Dimensional ◽  
Reynolds Numbers ◽  
Wake Flow ◽  
Recirculation Region ◽  
Two Dimensional ◽  
Number Range ◽  
Rotation Rates ◽  
Transition Mechanism ◽  
Three Dimensional Simulations

A study investigating the flow around a cylinder rolling or sliding on a wall has been undertaken in two and three dimensions. The cylinder motion is specified from a set of five discrete rotation rates, ranging from prograde through to retrograde rolling. A Reynolds number range of 20–500 is considered. The effects of the nearby wall and the imposed body motion on the wake structure and dominant wake transitions have been determined. Prograde rolling is shown to destabilize the wake flow, while retrograde rotation delays the onset of unsteady flow to Reynolds numbers well above those observed for a cylinder in an unbounded flow.Two-dimensional simulations show the presence of two recirculation zones in the steady wake, the lengths of which increase approximately linearly with the Reynolds number. Values of the lift and drag coefficient are also reported for the steady flow regime. Results from a linear stability analysis show that the wake initially undergoes a regular bifurcation from a steady two-dimensional flow to a steady three-dimensional wake for all rotation rates. The critical Reynolds number Rec of transition and the spanwise wavelength of the dominant mode are shown to be highly dependent on, but smoothly varying with, the rotation rate of the cylinder. Varying the rotation from prograde to retrograde rolling acts to increase the value of Rec and decrease the preferred wavelength. The structure of the fully evolved wake mode is then established through three-dimensional simulations. In fact it is found that at Reynolds numbers only marginally (~5%) above critical, the three-dimensional simulations indicate that the saturated state becomes time dependent, although at least initially, this does not result in a significant change to the mode structure. It is only at higher Reynolds numbers that the wake undergoes a transition to vortex shedding.An analysis of the three-dimensional transition indicates that it is unlikely to be due to a centrifugal instability despite the superficial similarity to the flow over a backward-facing step, for which the transition mechanism has been speculated to be centrifugal. However, the attached elongated recirculation region and distribution of the spanwise perturbation vorticity field, and the similarity of these features with those of the flow through a partially blocked channel, suggest the possibility that the mechanism is elliptic in nature. Some analysis which supports this conjecture is undertaken.

scholarly journals Instabilities within Rotating mode-2 Internal Waves

2017 ◽  
Author(s):  
David Deepwell ◽  
Marek Stastna ◽  
Aaron Coutino
Keyword(s):  
Three Dimensional ◽  
Side Wall ◽  
Kelvin Waves ◽  
Kelvin Wave ◽  
Rotation Rates ◽  
Mode 2 ◽  
Schmidt Numbers ◽  
Poincare Waves ◽  
The Right ◽  
Three Dimensional Simulations

Abstract. We present high resolution, three dimensional simulations of rotation modified mode-2 internal solitary waves at various rotation rates and Schmidt numbers. Rotation is seen to change the internal solitary-like waves observed in the absence of rotation into a leading Kelvin wave followed by Poincaré waves. Mass and energy is found to be advected towards the right-most side wall (for Northern hemisphere rotation) which led to Kelvin-Helmholtz instabilities within the leading Kelvin wave that form above and below the pycnocline. These instabilities are localized within a region near the side wall and intensify in vigour with increasing rotation rate. Secondary Kelvin waves form further behind the wave from either resonance with radiating Poincaré waves or the remnants of the K-H instability. The first of these mechanisms is in accord with published work on mode-1 Kelvin waves. Both types of secondary Kelvin waves form on the same side of the channel as the leading Kelvin wave. Comparisons of equivalent cases with different Schmidt numbers indicate that while low Schmidt number results in the correct general characteristics of the modified ISWs, it does not correctly predict the trailing Poincaré wave field or the intensity and duration of the K-H instabilities.

scholarly journals Can the Local Bubble explain the radio background?

2021 ◽  
Vol 502 (2) ◽  
pp. 2807-2814
Author(s):  
Martin G H Krause ◽  
Martin J Hardcastle
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Radio Emission ◽  
Magnetic Energy ◽  
Cosmic Ray ◽  
Observational Constraints ◽  
Local Bubble ◽  
Magnetic Energy Density ◽  
Magnetic Field Model ◽  
Radio Background

ABSTRACT The ARCADE 2 balloon bolometer along with a number of other instruments have detected what appears to be a radio synchrotron background at frequencies below about 3 GHz. Neither extragalactic radio sources nor diffuse Galactic emission can currently account for this finding. We use the locally measured cosmic ray electron population, demodulated for effects of the Solar wind, and other observational constraints combined with a turbulent magnetic field model to predict the radio synchrotron emission for the Local Bubble. We find that the spectral index of the modelled radio emission is roughly consistent with the radio background. Our model can approximately reproduce the observed antenna temperatures for a mean magnetic field strength B between 3 and 5 nT. We argue that this would not violate observational constraints from pulsar measurements. However, the curvature in the predicted spectrum would mean that other, so far unknown sources would have to contribute below 100 MHz. Also, the magnetic energy density would then dominate over thermal and cosmic ray electron energy density, likely causing an inverse magnetic cascade with large variations of the radio emission in different sky directions as well as high polarization. We argue that this disagrees with several observations and thus that the magnetic field is probably much lower, quite possibly limited by equipartition with the energy density in relativistic or thermal particles (B = 0.2−0.6 nT). In the latter case, we predict a contribution of the Local Bubble to the unexplained radio background at most at the per cent level.

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