TEMPORAL POWER SPECTRA OF THE HORIZONTAL VELOCITY OF THE SOLAR PHOTOSPHERE

We have derived the temporal power spectra of the horizontal velocity of the solar photosphere. The data sets for 14 quiet regions observed with the G-band filter of Hinode/SOT are analyzed to measure the temporal fluctuation of the horizontal velocity by using the local correlation tracking (LCT) method. Among the high resolution (similar to 0.'' 2) and seeing-free data sets of Hinode/SOT, we selected the observations whose duration is longer than 70 minutes and cadence is about 30 s. The so-called k-omega diagrams of the photospheric horizontal velocity are derived for the first time to investigate the temporal evolution of convection. The power spectra derived from k-omega diagrams typically have a double power-law shape bent over at a frequency of 4.7 mHz. The power-law index in the high frequency range is -2.4, while the power-law index in the low frequency range is -0.6. The root mean square of the horizontal speed is about 1.1 km s(-1) when we use a tracer size of 0.'' 4 in the LCT method. Autocorrelation functions of intensity fluctuation, horizontal velocity, and its spatial derivatives are also derived in order to measure the correlation time of the stochastic photospheric motion. Since one of the possible energy sources of the coronal heating is the photospheric convection, the power spectra derived in the present study will be of high value to quantitatively justify various coronal heating models.