scholarly journals High Resolution 3D Relativistic MHD Simulations of Jets

2009 ◽  
Vol 5 (H15) ◽  
pp. 254-255
Author(s):  
A. Ferrari ◽  
A. Mignone ◽  
P. Rossi ◽  
G. Bodo ◽  
S. Massaglia
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Numerical Simulations ◽  
Three Dimensional ◽  
Full Length ◽  
Toroidal Field ◽  
Toroidal Magnetic Field ◽  
Mhd Simulations ◽  
Strong Current

AbstractWe performed high-resolution three dimensional numerical simulations of relativistic MHD jets carrying an initially toroidal magnetic field responsible for the process of jet acceleration and collimation. We find that in the 3D case the toroidal field gives rise to strong current driven kink instabilities leading to jet wiggling. However, it appears to be able to maintain an highly relativistic spine along its full length.

Study of starspots in fully convective stars using three dimensional MHD simulations

2018 ◽  
Vol 13 (S340) ◽  
pp. 303-304
Author(s):  
Arnab Basak ◽  
Dibyendu Nandy
Keyword(s):  
High Resolution ◽  
Numerical Simulations ◽  
High Latitude ◽  
Three Dimensional ◽  
Stellar Dynamics ◽  
The Sun ◽  
Dynamo Action ◽  
Magnetic Structures ◽  
Mhd Simulations ◽  
Self Consistent

AbstractConcentrated magnetic structures such as sunspots and starspots play a fundamental role in driving solar and stellar activity. However, as opposed to the sun, observations as well as numerical simulations have shown that stellar spots are usually formed as high-latitude patches extended over wide areas. Using a fully spectral magnetohydrodynamic (MHD) code, we simulate polar starspots produced by self-consistent dynamo action in rapidly rotating convective shells. We carry out high resolution simulations and investigate various properties related to stellar dynamics which lead to starspot formation.

scholarly journals Simulations of Core Convection Dynamos in Rotating A-type Stars

2004 ◽  
Vol 215 ◽  
pp. 376-377
Author(s):  
Matthew Browning ◽  
Allan Sacha Brun ◽  
Juri Toomre
Keyword(s):  
Magnetic Field ◽  
Numerical Simulations ◽  
Differential Rotation ◽  
Three Dimensional ◽  
Dynamo Action ◽  
The Core ◽  
Core Convection ◽  
Seed Field ◽  
Initial Seed ◽  
Three Dimensional Simulations

We have conducted preliminary numerical simulations of a core convection dynamo operating within an A-type star of two solar masses. Convection within the core clearly can admit magnetic dynamo action. Magnetic field strengths in our three-dimensional simulations grow by many orders of magnitude, from an initial seed field to kilo-Gauss levels. We discuss the differential rotation and magnetic field sustained in our simulations.

Stability of electron inertia Alfvén solitons

1992 ◽  
Vol 48 (2) ◽  
pp. 335-343 ◽  
Author(s):  
P. Frycz ◽  
R. Rankin ◽  
J. C. Samson
Keyword(s):  
Magnetic Field ◽  
Numerical Simulations ◽  
Final Stage ◽  
Wave Breaking ◽  
Characteristic Length ◽  
Three Dimensional ◽  
Soliton Solutions ◽  
Dimensional Electron ◽  
Electron Inertia ◽  
Nonlinear Phase

Das, Kamp and Sluijter have proposed equations describing three-dimensional electron inertia Alfvén waves for which the characteristic length scales in directions parallel and perpendicular to the ambient magnetic field are of the same order. Planar, obliquely propagating soliton solutions of these equations are known to be linearly unstable. Numerical simulations reveal the nonlinear phase of the evolution of these solitons: a transition from flat to cylindrical solitons is observed, followed by breaking-up into three-dimensional localized cavities. The final stage corresponds to wave breaking; no final stable structure is achieved within the model.

Three-dimensional numerical simulations of susceptibility-induced magnetic field inhomogeneities in the human head

2002 ◽  
Vol 20 (10) ◽  
pp. 759-770 ◽  
Author(s):  
Trong-Kha Truong ◽  
Bradley D. Clymer ◽  
Donald W. Chakeres ◽  
Petra Schmalbrock
Keyword(s):  
Magnetic Field ◽  
Numerical Simulations ◽  
Three Dimensional ◽  
Human Head ◽  
Induced Magnetic Field

scholarly journals Generation of Strong Toroidal Magnetic Field Near the Bottom of the Solar Convective Zone

1993 ◽  
Vol 137 ◽  
pp. 78-80
Author(s):  
V.N. Krivodubskij
Keyword(s):  
Magnetic Field ◽  
Angular Velocity ◽  
Magnetic Induction ◽  
Convective Zone ◽  
Generation Mechanism ◽  
Toroidal Field ◽  
Toroidal Magnetic Field ◽  
Poloidal Magnetic Field ◽  
Radial Gradient ◽  
Magnetic Buoyancy

AbstractThe generation mechanism of the toroidal magnetic field by the angular velocity radial gradient acting on the relict poloidal magnetic field on the boundary between the con-vective and radiative zones is proposed. The magnetic induction magnitude of the toroidal field reaches about 2×10σ G, the limiting effect of the magnetic buoyancy being taking into account. This value conforms to the estimation of toroidal field obtained from helioseismological data.

scholarly journals On MHD rotational transport, instabilities and dynamo action in stellar radiation zones

2008 ◽  
Vol 4 (S259) ◽  
pp. 421-422
Author(s):  
Stéphane Mathis ◽  
A.-S. Brun ◽  
J.-P. Zahn
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
High Resolution ◽  
Magnetic Fields ◽  
Transport Processes ◽  
Dynamo Action ◽  
Mhd Instability ◽  
Mhd Simulations ◽  
Stellar Radiation ◽  
Magnetic Transport

AbstractMagnetic field and their related dynamical effects are thought to be important in stellar radiation zones. For instance, it has been suggested that a dynamo, sustained by a m = 1 MHD instability of toroidal magnetic fields (discovered by Tayler in 1973), could lead to a strong transport of angular momentum and of chemicals in such stable regions. We wish here to recall the different magnetic transport processes present in radiative zone and show how the dynamo can operate by recalling the conditions required to close the dynamo loop (BPol → BTor → BPol). Helped by high-resolution 3D MHD simulations using the ASH code in the solar case, we confirm the existence of the m = 1 instability, study its non-linear saturation, but we do not detect, up to a magnetic Reylnods number of 105, any dynamo action.

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