Correlation between decimetric radio emission and hard X-rays in solar flares

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Table 4:

Parameters of the regression analysis between delay and X-ray flux.
	Pulsations				Spikes
	RHESSI		GOES		RHESSI		GOES
	Gauss	Maximum	Gauss	Maximum	Gauss	Maximum	Gauss	Maximum
Intercept coefficient (a)	149.8	162.6	$1.1\times10^{-5}$	$1.13\times10^{-5}$	93.9	100.2	$5.2\times10^{-6}$	$5.7\times10^{-6}$
Standard deviation intercept ( $\Delta$ a)	33.4	38.5	$1.8\times10^{-6}$	$1.5\times10^{-6}$	28.0	30.8	$1.6\times10^{-6}$	$1.9\times10^{-6}$
Slope coefficient (b)	9.1	14.8	$3.3\times10^{-6}$	$2.8\times10^{-6}$	-17.6	-17.6	$-3.2\times10^{-6}$	$-3.5\times10^{-6}$
Standard deviation slope ( $\Delta$ b)	7.5	9.9	$1.0\times10^{-6}$	$4.3\times10^{-7}$	3.7	3.2	$5.6\times10^{-7}$	$8.7\times10^{-7}$

Note: The delay of the X-rays is determined from the cross-correlation between decimetric pulsations and spikes with HXR flux (Tables 1 and 2). Linear regression is applied and the bisector reported. The function has the form $f=a+b\tau$ , where f is the X-ray flux (RHESSI for hard X-ray and GOES for soft X-ray) and $\tau$ is the delay using the Gauss or maximum method.

Source LaTeX | All tables | In the text

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