A Model For Pulsed Radio Cmi Emission From Ultra Cool Dwarfs

Details A Model For Pulsed Radio Cmi Emission From Ultra Cool Dwarfs A Model For Pulsed Radio Cmi Emission From Ultra Cool Dwarfs

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21934530l&link_type=abstract

American Astronomical Society, AAS Meeting #219, #345.30

Astronomy and Astrophysics

Astronomy

Scientific paper

Pulsed radio emission has been detected from several from rapidly rotating ultra cool dwarfs (UCD's). The pulses are short-duration, highly circularly polarized, have a pulse period approximately equal to the stellar rotation period, and a phase that depends on frequency. These characteristics can be explained by cyclotron maser instability (CMI) emission from the polar regions of a co-rotating magnetosphere that is obliquely oriented w.r.t. the star's rotation axis. I present 3-dimensional ray-tracing results for CMI-generated radiation at the local cyclotron frequency that account for all major observed features of the pulsed emission.

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