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Hallinan, G,Doyle, G,Antonova, A,Bourke, S,Jardine, M,Donati, JF,Morin, J,Golden, A,Stempels, E
Mapping the Radio Coronae of Cool Stars and Brown Dwarfs
COOL STARS, STELLAR SYSTEMS AND THE SUN
2009
September
Published
1
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Optional Fields
Radiation Mechanisms: Nonthermal Radio Continuum: Stars Stars: Activity Stars: Low-Mass Brown Dwarfs Stars: Magnetic Fields FULLY CONVECTIVE STAR MAGNETIC-FIELD EMISSION TVLM-513-46546
146
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The pulsing, radio emission detected from ultracool dwarfs can be used as a powerful diagnostic of magnetic field strengths and topologies at and below the substellar boundary. Studies thus far have confirmed magnetic field strengths of 3 kG for two late M dwarfs and 1.7 kG for an L3.5 dwarf, the latter being the first confirmation of kG magnetic fields for an L dwarf. Ongoing long term monitoring of the radio pulses will also investigate the stability of the associated large-scale magnetic fields over timescales > 1 Year. We also present the preliminary results of a lengthy radio monitoring campaign of the rapidly rotating M4 star V374 Peg, with the resulting light cures phased with magnetic maps previously obtained through Iceman Doppler Imaging. The radio emission from V374 peg is strongly modulated by the large kale dipolar magnetic field. with two clear peaks in the radio light curve per period of rotation, occurring when the dipolar field lies in the plane of the sky. These results provide strong evidence that the electron cyclotron maser instability plays a pivotal role in the production of quiescent radio emission from V374 Peg. representing a significant departure from the accepted model of gyrosynchrotron emission as the dominant source of quiescent radio emission from active M dwarfs.
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