Flare Observations with GONG

The X10 flare in AR 10486 on 29 October 2003 displayed significant magnetic field and 'white light' changes. The signature of the flare is clearly visible as a 30% increase in intensity, accompanied by a 50% decrease in the line strength and significant changes in the magnetic flux strength and configuration. The image at left shows intensity (left), line strength (middle) and magnetic (right) changes at one minute intervals centered around the peak of the flare, with respect to a reference frame about 20 minutes before the flare.

The movie shows the evolution of the intensity (top left), line strength (top right), magnetic field strength (bottom left) and Doppler velocity (bottom right), after subtraction of the reference frame.

The top panels show the change in the intensity I, line strength M and magnetic field strength B at the peak of the flare with respect to the reference frame; the bottom panels show the temporal variation of each quantity at the pixel marked by a cross in the images.

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	The X10 flare in AR 10486 on 29 October 2003 displayed significant magnetic field and 'white light' changes. The signature of the flare is clearly visible as a 30% increase in intensity, accompanied by a 50% decrease in the line strength and significant changes in the magnetic flux strength and configuration. The image at left shows intensity (left), line strength (middle) and magnetic (right) changes at one minute intervals centered around the peak of the flare, with respect to a reference frame about 20 minutes before the flare.
	The movie shows the evolution of the intensity (top left), line strength (top right), magnetic field strength (bottom left) and Doppler velocity (bottom right), after subtraction of the reference frame.
	The top panels show the change in the intensity I, line strength M and magnetic field strength B at the peak of the flare with respect to the reference frame; the bottom panels show the temporal variation of each quantity at the pixel marked by a cross in the images.