Self‐consistent turbulent dynamo modeling of reversed field pinches and planetary magnetic fields

1990 ◽  
Vol 2 (7) ◽  
pp. 1589-1600 ◽  
Author(s):  
Akira Yoshizawa
Keyword(s):  
Magnetic Fields ◽  
Turbulent Dynamo ◽  
Self Consistent ◽  
Planetary Magnetic Fields ◽  
Reversed Field

High-Performance Modelling in Geodynamics

2012 ◽  
pp. 324-352 ◽  
Author(s):  
Lena Noack ◽  
Nicola Tosi
Keyword(s):  
Magnetic Fields ◽  
High Performance ◽  
The Self ◽  
Performance Modelling ◽  
Tectonic Plates ◽  
Multi Scale ◽  
Core Convection ◽  
Self Consistent ◽  
Planetary Magnetic Fields ◽  
Geodynamic Processes

Modelling of geodynamic processes like mantle or core convection has strongly improved over the last two decades thanks to the steady development of numerical codes that tend to incorporate a more and more realistic physics. High-performance parallel computations allow the simulation of complex problems, such as the self-consistent generation of tectonic plates or the formation of planetary magnetic fields. However, the need to perform broad explorations of the parameter space and the large computational demands imposed by the non-linear, multi-scale nature of convection, requires several simplifications, in the domain geometry as well as in the physical complexity of the problem. In this chapter, the authors give an overview of the state-of-the-art convection simulations in planetary mantles, the different models and geometries used, and various methods to simplify the computations.

scholarly journals Planetary Magnetic Fields and Habitability in Super Earths

2018 ◽  
Vol 27 (1) ◽  
pp. 183-231 ◽  
Author(s):  
Pablo Cuartas-Restrepo
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Scaling Laws ◽  
Thermal Evolution ◽  
Solid Core ◽  
Direct Influence ◽  
Physical Processes ◽  
Planetary Magnetic Fields ◽  
Planetary Magnetic Field ◽  
Planetary Dynamos

Abstract This work seeks to summarize some special aspects of a type of exoplanets known as super-Earths (SE), and the direct influence of these aspects in their habitability. Physical processes like the internal thermal evolution and the generation of a protective Planetary Magnetic Field (PMF) are directly related with habitability. Other aspects such as rotation and the formation of a solid core are fundamental when analyzing the possibilities that a SE would have to be habitable. This work analyzes the fundamental theoretical aspects on which the models of thermal evolution and the scaling laws of the planetary dynamos are based. These theoretical aspects allow to develop models of the magnetic evolution of the planets and the role played by the PMF in the protection of the atmosphere and the habitability of the planet.

Planetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution

2007 ◽  
Vol 129 (1-3) ◽  
pp. 245-278 ◽  
Author(s):  
Rickard Lundin ◽  
Helmut Lammer ◽  
Ignasi Ribas
Keyword(s):  
Magnetic Fields ◽  
Solar Forcing ◽  
Atmospheric Evolution ◽  
Planetary Magnetic Fields

Response : Planetary Magnetic Fields and Rotation

Science ◽  
1967 ◽  
Vol 158 (3801) ◽  
pp. 674-674
Author(s):  
J. A. Van Allen
Keyword(s):  
Magnetic Fields ◽  
Planetary Magnetic Fields

Planetary Magnetic Fields and Rotation

Science ◽  
1967 ◽  
Vol 158 (3801) ◽  
pp. 674-674
Author(s):  
Robert T. Brown
Keyword(s):  
Magnetic Fields ◽  
Planetary Magnetic Fields

Planetary Magnetic Fields and Rotation

Science ◽  
1967 ◽  
Vol 158 (3801) ◽  
pp. 674-674
Author(s):  
Robert T. Brown
Keyword(s):  
Magnetic Fields ◽  
Planetary Magnetic Fields

scholarly journals Sturm und Drang: The turbulent, magnetic tempest in the Galactic center

2013 ◽  
Vol 9 (S303) ◽  
pp. 395-398
Author(s):  
Brian C. Lacki
Keyword(s):  
Magnetic Fields ◽  
Galactic Halo ◽  
Galactic Center ◽  
Termination Shock ◽  
Strong Magnetic Fields ◽  
Random Forcing ◽  
Sturm Und Drang ◽  
Turbulent Dynamo ◽  
Starburst Regions

AbstractThe Galactic center central molecular zone (GCCMZ) bears similarities with extragalactic starburst regions, including a high supernova (SN) rate density. As in other starbursts like M82, the frequent SNe can heat the ISM until it is filled with a hot (∼ 4 × 107 K) superwind. Furthermore, the random forcing from SNe stirs up the wind, powering Mach 1 turbulence. I argue that a turbulent dynamo explains the strong magnetic fields in starbursts, and I predict an average B ∼70 μG in the GCCMZ. I demonstrate how the SN driving of the ISM leads to equipartition between various pressure components in the ISM. The SN-heated wind escapes the center, but I show that it may be stopped in the Galactic halo. I propose that the Fermi bubbles are the wind's termination shock.

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