Properties of Magnetohydrodynamic Waves in the Solar Photosphere Obtained Withhinode

We report the observations of the magneto-hydrodynamic waves propagating along magnetic flux tubes in the solar photosphere. We identified 20 isolated strong peaks (8 peaks for pores and 12 peaks for inter-granular magnetic structure) in the power spectra of the l.o.s. (line-of-sight) magnetic flux, the l.o.s. velocity, and the intensity for 14 different magnetic concentrations. The observation is performed with the spectro-polarimeter of the Solar Optical Telescope aboard the Hinode satellite. The oscillation periods are located in 3−6 min for the pores and in 4−9 min for the inter-granular magnetic elements. These peaks correspond to the magnetic, the velocity, and the intensity fluctuation in time domain with r.m.s. (root mean square) amplitudes of 4 − 17 G (0.3 − 1.2 %), 0.03 − 0.12 km s−1, and 0.1 − 1%, respectively. Phase differences between the l.o.s. magnetic flux (φB), the l.o.s. velocity (φv), the intensities of the line core (φI,core), and the continuum intensity (φI,cont) have striking concentrations at around −90 ◦ for φB − φv and φv − φI,core, around 180 ◦ for φI,core − φB, and