The Morphology of Decimetric Emission from Solar Flares: GMRT Observations
| Autor: | Stephen M. White, V. I. Garaimov, P. Janardhan, S. Ananthakrishnan, Prasad Subramanian, M. R. Kundu |
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| Rok vydání: | 2006 |
| Předmět: |
Physics
Photosphere Solar flare Astrophysics::High Energy Astrophysical Phenomena Astronomy Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Magnetic field law.invention Nanoflares Radio telescope Wavelength Space and Planetary Science law Physics::Space Physics Astrophysics::Solar and Stellar Astrophysics Microwave Flare |
| Zdroj: | Solar Physics. 236:369-387 |
| ISSN: | 1573-093X 0038-0938 |
| DOI: | 10.1007/s11207-006-0059-8 |
| Popis: | 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˚. |
| Databáze: | OpenAIRE |
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