The Morphology of Decimetric Emission from Solar Flares: GMRT Observations |
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| Authors: | M R Kundu S M White V I Garaimov P Subramanian S Ananthakrishnan P Janardhan |
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| Institution: | (1) Astronomy Department, University of Maryland, College Park, MD, 20742, U.S.A.;(2) Special Astrophysical Observatory, St. Petersburg Branch, Russian Academy of Sciences, St. Petersburg, 196140, Russia;(3) Inter-University Centre for Astronomy and Astrophysics, P.O. Bag 4, Ganeshkhind, Pune, 411007, India;(4) National Centre for Radio Astrophysics, TIFR, P.O. Bag 3, Ganeshkhind, Pune, 411007, India;(5) Astronomy and Astrophysics Division, Physical Research Laboratory, Navrang-pura, Ahmedabad, 380009, India |
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| Abstract: | Observations of a solar flare at 617 MHz with the Giant Meter-wave Radio Telescope (GMRT) are used to study the morphology
of flare radio emission at decimetric wavelengths. There has been very little imaging in the 500 – 1000 MHz frequency range,
but it is of great interest, since it corresponds to densities at which energy is believed to be released in solar flares.
This event has a very distinctive morphology at 617 MHz: the radio emission is clearly resolved by the 30″ beam into arc-shaped
sources seeming to lie at the tops of long loops, anchored at one end in the active region in which the flare occurs, with
the other end lying some 200 000 km away in a region of quiet solar atmosphere. Microwave images show fairly conventional
behaviour for the flare in the active region: it consists of two compact sources overlying regions of opposite magnetic polarity
in the photosphere. The decimetric emission is confined to the period leading up to the impulsive phase of the flare, and
does not extend over a wide frequency range. This fact suggests a flare mechanism in which the magnetic field at considerable
height in the corona is destabilized a few minutes prior to the main energy release lower in the corona. The radio morphology
also suggests that the radiating electrons are trapped near the tops of magnetic loops, and therefore may have pitch angles
near 90˚. |
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