Determining Core Properties From a Planet's Magnetic Field Morphology

Details Determining Core Properties From a Planet's Magnetic Field Morphology Determining Core Properties From a Planet's Magnetic Field Morphology

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmgp41c..02s&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #GP41C-02

Other

1507 Core Processes (1213, 8115), 1510 Dynamo: Theories And Simulations, 1595 Planetary Magnetism: All Frequencies And Wavelengths, 5440 Magnetic Fields And Magnetism, 5734 Magnetic Fields And Magnetism

Scientific paper

Determining properties of a planet's deep interior are difficult because we cannot observe this region directly as we can the surface of a planet. On Earth, seismology has provided important information on the structure and composition of the deep interior including the core. In addition, properties of the Earth's outer core motions have been determined mostly from observations of the geomagnetic field secular variation. Unfortunately we are not at present able to conduct detailed seismic studies and observations of magnetic field secular variation for other planets to provide us with the same quality of information on their cores. We are however, capable of studying a planet's magnetic field morphology quite extensively with an orbiting spacecraft at relatively low altitude. Here we use numerical dynamo models to determine what magnetic field structures can tell us about a planet's core. We concentrate on properties such as inner core size and outer core convective vigor. The results are used to determine what key observations of magnetic field structures could be made by future spacecraft missions to provide information on the dynamo source regions inside planets. This type of study can aid in determining the internal structure and evolution of Mercury, Jupiter, Saturn and Ganymede for which little is known about these properties.

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