Abstract
The intensity and frequency spectrum of gyro-synchrotron emission from energetic solar electrons radiating in coronal magnetic fields are calculated. These calculations, based on a recent study of the generation of gyro-synchrotron emission in a magnetoactive plasma, are applied to a Type IV radio burst originating at a high altitude in the solar corona. It is shown that the observed frequency spectrum of the burst, which exhibits very sharp low and high frequency cutoffs, can be best understood in terms of gyro-synchrotron emission in an ionized medium and that from the observed frequency spectrum and the ambient coronal density it is possible to deduce both the magnetic field at the site of the emission and the range of electron energies responsible for the burst.
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NAS-NASA Post-Doctoral Resident Research Associate.
Research supported by the National Research Foundation under grant GP-849.
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Ramaty, R., Lingenfelter, R.E. Determination of the coronal magnetic field and the radio-emitting electron energy from a Type IV solar radio burst. Sol Phys 5, 531–545 (1968). https://doi.org/10.1007/BF00147018
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DOI: https://doi.org/10.1007/BF00147018