Table 4: Slopes of the linear fits to the logarithm of the mean weighted PWTs for sub-samples of the analysed stars and without any correction for the magnitude of the stars.
Spectral Slope from $1.0 \times 10^{-4}$ Slope from $0.7 \times 10^{-3}$

type to $0.6 \times 10^{-3}$ Hz to $2.5 \times 10^{-3}$ Hz

F $-0.618 \pm 0.021$ $-0.519\pm 0.006$

G $-0.561 \pm 0.017$ $-0.419\pm 0.007$

K $-0.639 \pm 0.023$ $-0.573\pm 0.013$

M $-0.653 \pm 0.018$ $-0.582\pm 0.007$

**Table 4:** Slopes of the linear fits to the logarithm of the mean weighted PWTs for sub-samples of the analysed stars and without any correction for the magnitude of the stars.
Spectral	Slope from $1.0 \times 10^{-4}$	Slope from $0.7 \times 10^{-3}$
type	to $0.6 \times 10^{-3}$ Hz	to $2.5 \times 10^{-3}$ Hz
F	$-0.618 \pm 0.021$	$-0.519\pm 0.006$
G	$-0.561 \pm 0.017$	$-0.419\pm 0.007$
K	$-0.639 \pm 0.023$	$-0.573\pm 0.013$
M	$-0.653 \pm 0.018$	$-0.582\pm 0.007$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Stellar data analysis
	3 Stellar acoustic Power Wavelet Transforms
	4 Analysis of a G type star: the Sun
	5 Discussion and conclusions
	References