Confirming Auroral Emissions on an Ultracool Dwarf

Details Confirming Auroral Emissions on an Ultracool Dwarf Confirming Auroral Emissions on an Ultracool Dwarf

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011noao.prop..584h&link_type=abstract

NOAO Proposal ID #2011A-0584

Physics

Scientific paper

Ultracool dwarf pulsars are a small group of very low-mass stars and brown dwarfs (collectively: ultracool dwarfs) which show highly coherent radio emission which is pulsed on the rotational period. The radio emission is providing a new framework within which to interpret the magnetic properties of ultracool, one in which the magnetic fields and radio emission has more in common with the magnetospheres of giant planets, than Sun-like stars. The best studied of these objects is TVLM 513-46546. It shows periodic optical emission, and recent observations suggest that this variabilty may be a dramatic manifestation of aurorae on an ultracool dwarf. Here we request time-resolved spectroscopy of TVLM 513-46546 to measure the optical spectrum of the variable emission. These results will allow us to establish 1) the true spectrum of the auroral emission, 2) the temperature difference between the hot spot and the photosphere of the dwarf and 3) the amount of energy expended in producing this auroral hot spot.

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