Microwave emission from a sunspot. I - Implications for the sunspot magnetic structure

Physics

Scientific paper

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Microwave Emission, Solar Corona, Solar Magnetic Field, Solar Physics, Solar Radio Emission, Sunspots, Brightness Temperature, Gyrofrequency, Magnetic Flux

Scientific paper

The magnetic field strength of a sunspot can be determined from the gyroresonance brightness temperature spectrum by using the property that microwave brightness is limited above a frequency given by an integer-multiple of the gyrofrequency. This concept is used to find the radial distribution of the magnetic field at the coronal base of a sunspot in the active region NOAA 4741. It is shown that the o-mode emission must arise primarily from the second harmonic of the gyrofrequency, and that the third harmonic is responsible for the x-mode emission. An expression is given to describe the radial distribution of magnetic fields at the coronal base of a sunspot. Coronal magnetic fields are found to originate mainly in the photospheric umbral region. Finally, while it is possible to approximate roughly the derived vertical variation of magnetic fields by means of a dipole model, the radial field distribution at coronal heights is determined to be more confined than predicted by this model.

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