The energy of waves in the photosphere and lower chromosphere

Abstract

We investigate the statistics of the intensity distributions as function of the wavelength for Ca II H and the CA II IR line at 854.2 nm to estimate the energy content. We derived the intensity variations at different heights of the solar atmosphere as given by the line wings and line cores of the two spectral lines. We converted the observed intensities to absolute energy units employing reference profiles calculated in NLTE. We also converted the observed intensity fluctuations to brightness temperatures assuming LTE. The rms fluctuations of the emitted intensity are about 0.6 (1.2) W/m2 ster pm near the core of the Ca IR line (Ca II H), corresponding to intensity fluctuations of about 20% (30%). For the line wing, we find rms values of about 0.3 W/ m2 ster pm for both lines, corresponding to relative fluctuations below 5%. The rms shows a local minimum for wavelengths forming at about 130 km height, but otherwise increases from the wing to the core. The rms brightness temperature fluctuations are below 100 K for the photosphere and up to 500 K in the chromosphere. The skewness of the intensity distributions is close to zero in the outer line wing and positive throughout the rest of the spectrum. The skewness shows a pronounced maximum on locations with photospheric magnetic fields for wavelengths in between the line wing and the line core, and a global maximum at the very core for both magnetic and field-free locations. The energy content of the intensity fluctuations is insufficient to create a similar temperature rise in the chromosphere as predicted in most reference models of the solar atmosphere. The enhanced skewness between photosphere and lower solar chromosphere on magnetic locations indicates a mechanism which solely acts on magnetized plasma.