Measuring the Earth's Synchrotron Emission from Radiation Belts with a Lunar Near Side Radio Array
arXiv:1912.04482 · doi:10.1029/2019RS006891
Abstract
The high kinetic energy electrons that populate the Earth's radiation belts emit synchrotron emissions because of their interaction with the planetary magnetic field. A lunar near side array would be uniquely positioned to image this emission and provide a near real time measure of how the Earth's radiation belts are responding to the current solar input. The Salammbo code is a physical model of the dynamics of the three-dimensional phase-space electron densities in the radiation belts, allowing the prediction of 1 keV to 100 MeV electron distributions trapped in the belts. This information is put into a synchrotron emission simulator which provides the brightness distribution of the emission up to 1 MHz from a given observation point. Using Digital Elevation Models from Lunar Reconnaissance Orbiter (LRO) Lunar Orbiter Laser Altimeter (LOLA) data, we select a set of locations near the Lunar sub-Earth point with minimum elevation variation over various sized patches where we simulate radio receivers to create a synthetic aperture. We consider all realistic noise sources in the low frequency regime. We then use a custom CASA code to image and process the data from our defined array, using SPICE to align the lunar coordinates with the Earth. We find that for a moderate lunar surface electron density of 250/cm^3, the radiation belts may be detected every 12-24 hours with a 16384 element array over a 10 km diameter circle. Changing electron density can make measurements 10x faster at lunar night, and 10x slower at lunar noon.
arXiv comment23 pages plus references. 3 Tables, 6 Figures
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