Radio Emission from Extrasolar Planetary Systems

Details Radio Emission from Extrasolar Planetary Systems Radio Emission from Extrasolar Planetary Systems

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....3834f&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #3834

Physics

Scientific paper

Each of the gas giants in our solar system and the Earth possess planetary-scale magnetic fields, generated by internal dynamo currents. The magnetic polar regions of these solar system 'magnetic planets' produce intense, aurora-related radio emission, generated via coherent cyclotron radiation from solar-wind powered electron currents. Simple scaling laws suggest that Jovian-mass planets close to their host stars should produce radio emission; detecting such emission would be the first direct detection of these planetary systems. We describe a series of Very Large Array (VLA) observations of extrasolar planets, largely using its 74 MHz observing system. The predicted emission frequencies of extrasolar planet radio emission depend upon the (unknown) magnetic moments and rotation rates of the planets. Scaling from Jovian properties, it seems likely that many extrasolar planets will emit below ~100 MHz, making observations at 74 MHz a useful first effort. Our current limits are close to, but generally just above that predicted for the radiative power from planetary cyclotron emission. We discuss the implications that the existing observations have for the planet's radio emission, and hence on the planetary magnetic field and stellar wind environment, as well as the possibility for far more stringent observational limits with the Low Frequency Array (LOFAR).

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