Open AccessSimulations of coronal type III solar radio bursts: 3. Effects of beam and coronal parameters
Author(s) -
Li Bo,
Cairns Iver H.,
Robinson Peter A.
Publication year - 2009
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2008ja013687
Subject(s) - physics , astrophysics , corona (planetary geology) , brightness temperature , coronal hole , electron temperature , brightness , plasma , computational physics , radiation , solar wind , coronal mass ejection , astronomy , optics , astrobiology , quantum mechanics , venus
A recently developed simulation model is used to investigate the effects of varying the coronal and electron heating conditions on the dynamic spectra of coronal type III bursts (70–370 MHz) observed at Earth. The flux of 2 f p emission is significantly higher than that of f p emission, which is unlikely to be observable except under very favorable propagation conditions. Moreover, the 2 f p emission is unlikely to continue into the solar wind, although some bursts are very strong and will extend into the upper corona with lower frequencies than simulated, consistent qualitatively with observations. The flux and brightness temperature of 2 f p emission are affected significantly by variations in the parameters, while the frequency drift rate and half‐power duration are affected only weakly. Further, the simulations confirm the standard interpretation of the drift rate of 2 f p emission in terms of the plasma density profile and a characteristic beam speed that agrees quantitatively with the simulated beam dynamics for wide ranges of coronal and heating conditions. For weak heating events or events with high coronal electron temperature, the remote radiation shows characteristics that agree quantitatively with microbursts. When the heating is even weaker and/or the electron temperature is even higher, the heating events are radio quiet, consistent qualitatively with hard X‐ray observations. For similar heating originating in similar frequency ranges, different density models yield quantitatively similar results except for the drift rate. Variations of the levels of a given density profile, corresponding to background corona or coronal streamers, can also cause significant changes in spectral characteristics.