Magnetic communication scenarii for close-in extrasolar planets

Details Magnetic communication scenarii for close-in extrasolar planets Magnetic communication scenarii for close-in extrasolar planets

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006tafp.conf..274p&link_type=abstract

"Tenth Anniversary of 51 Peg-b: Status of and prospects for hot Jupiter studies. Colloquium held at Observatoire de Haute Proven

Physics

1

Scientific paper

Close-in extrasolar planetary systems are often considered to be scaled up versions of Jupiter and its satellite, Io, which exhibit a strong electromagnetic interaction. Still, this scenario lacks detailed modeling to show its feasibility. We try to fill this gap by studying the magnetic interaction of close-in extrasolar planes and their stars on the basis of realistic stellar wind models and numerical simulations in the frame of resistive magneto-hydrodynamics. We find that a current system between the planet and its star may be established. Contrary to Io and Jupiter it seems to be unlikely that the flux tubes connecting the planet and the star are the source region for radio emissions due to a cyclotron maser instability. Therefore, we suggest that the energy contained in the current system may be dissipated in the chromosphere of the star. This is indicated by observations of an enhanced chromospheric activity on HD 179949.

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