Table 1: Slopes of the linear fits to the logarithm of the mean weighted PWTs 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 $-0.600 \pm 0.019$ $-0.502\pm 0.006$

G $-0.513 \pm 0.015$ $-0.351\pm 0.006$

K $-0.656 \pm 0.019$ $-0.579\pm 0.011$

M $-0.724 \pm 0.016$ $-0.567\pm 0.013$

**Table 1:** Slopes of the linear fits to the logarithm of the mean weighted PWTs 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	$-0.600 \pm 0.019$	$-0.502\pm 0.006$
G	$-0.513 \pm 0.015$	$-0.351\pm 0.006$
K	$-0.656 \pm 0.019$	$-0.579\pm 0.011$
M	$-0.724 \pm 0.016$	$-0.567\pm 0.013$

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