scholarly journals A method for remote sensing of weak planetary magnetic fields: Simulated application to Mars

2013 ◽  
Vol 40 (19) ◽  
pp. 5014-5018 ◽  
Author(s):  
Richard Larsson ◽  
Robin Ramstad ◽  
Jana Mendrok ◽  
Stefan Alexander Buehler ◽  
Yasuko Kasai
2018 ◽  
Vol 27 (1) ◽  
pp. 183-231 ◽  
Author(s):  
Pablo Cuartas-Restrepo

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.


2007 ◽  
Vol 129 (1-3) ◽  
pp. 245-278 ◽  
Author(s):  
Rickard Lundin ◽  
Helmut Lammer ◽  
Ignasi Ribas

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

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

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

The paper shows that a planetary magnetic field expressed in the conventional form of a spherical harmonic expanson can be completely represented by the vector sum of fields produced by a set of magnetic dipoles with different magnetic moments, tilted from the planetary spin axis and offset from the planetary centre by different amounts. For convenience, the transformation from multipole systems to dipole systems is restricted to that from multipoles up to octupole to five dipoles. The scalar equipotential transformation analytically results in 24 equations; these can be subsequently solved for the 24 adjustable parameters in dipole systems with the predetermined ‘main dipole’. The numerical comparison of the jovian magnetic field between the jovian O 4 and the five-dipole models reveals a very good agreement with the subtle details. It is obvious that this type of transformation would open up the simplest practical way to simulate planetary magnetic fields with the dipole patterns.


Eos ◽  
2014 ◽  
Vol 95 (38) ◽  
pp. 343-343
Author(s):  
Michael Purucker

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