Terrestrial AKR Growth Rates and Beaming: Implications for Extrasolar Planetary and Stellar Magnetospheric Radio Emission

Details Terrestrial AKR Growth Rates and Beaming: Implications for Extrasolar Planetary and Stellar Magnetospheric Radio Emission Terrestrial AKR Growth Rates and Beaming: Implications for Extrasolar Planetary and Stellar Magnetospheric Radio Emission

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm13a1658m&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM13A-1658

Physics

0689 Wave Propagation (2487, 3285, 4275, 4455, 6934), 2704 Auroral Phenomena (2407), 2756 Planetary Magnetospheres (5443, 5737, 6033), 6033 Magnetospheres (2756), 6296 Extra-Solar Planets

Scientific paper

Recent advances in our understanding of the electron cyclotron maser instability (CMI) in the Earth's magnetosphere are useful for predicting characteristics of low-frequency radio emission from extrasolar planets. In particular, the discovery that the CMI mechanism is likely driven by a shell-type velocity distribution rather than a loss-cone, and the narrow 'tangent-plane' angular beaming of the resulting radiation may have counterparts in Jovian-type planets both in our own solar system and in the many extrasolar planets discovered in the past 15 years. In addition, the recent discovery of periodic highly circularly polarized radiation from certain very late-type stars is most easily understood by a CMI mechanism which is narrowly beamed. I will discuss the plasma environmental conditions need to sustain the CMI mechanism and compare these constraints to what is presently known concerning extrasolar planetary and stellar magnetospheres.

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