Mapping radio emitting-region on low-mass stars and brown dwarfs

Details Mapping radio emitting-region on low-mass stars and brown dwarfs Mapping radio emitting-region on low-mass stars and brown dwarfs

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epjwc..1606013y&link_type=abstract

Research, Science and Technology of Brown Dwarfs and Exoplanets: Proceedings of an International Conference held in Shangai on O

Physics

Scientific paper

Strong magnetic activity in ultracool dwarfs (UCDs, spectral classes later than M7) have emerged from a number of radio observations, including the periodic beams. The highly (up to 100%) circularly polarized nature of the emission point to an effective amplification mechanism of the high-frequency electromagnetic waves - the electron cyclotron maser (ECM) instability. Several anisotropic velocity distibution models of electrons, including the horseshoe distribution, ring shell distribution and the loss-cone distribution, are able to generate the ECM instability. A magnetic-field-aligned electric potential would play an significant role in the ECM process. We are developing a theoretical model in order to simulate ECM and apply this model to map the radio-emitting region on low-mass stars and brown dwarfs.

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