Vertical propagation of waves in the solar atmosphere. I. Observations of phase delays

Journal Article · Sun Jul 15 04:00:00 EDT 1979 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157219· OSTI ID:6039340

Lites, B W; Chipman, E G

The Sacramento Peak Observatory Tower Vacuum Telescope, echelle spectrograph, and diode array were used to simultaneously measure velocities and intensities in three spectral lines and the continuum. According to our contribution function calculations, these wavelengths are formed at heights from the low photosphere to the chromosphere. The phase velocities of the intensity and velocity oscillations between the various heights, and the phase relations between intensity and velocity at one height were determined as a function of frequency in the range 0--11.1 mHz. The oscillations are found to be predominantly evanescent in nature for frequencies less than 4 mHz and propagating upward at higher frequencies, with phase velocities approaching the sound speed at approximately 6 mHz. We calculated the upward mechanical flux in the observed waves at two atmospheric heights by an integration in frequency, and we show that in the chromosphere the propagated power is centered at 6 MHz but is still much too small to heat the overlying atmosphere.

• Research Organization: Laboratory for Atmospheric and Space Physics, University of Colorado
• OSTI ID: 6039340
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 231:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
ATOMIC MODELS
CHROMOSPHERE
DISTRIBUTION FUNCTIONS
ENERGY SPECTRA
MATHEMATICAL MODELS
OSCILLATIONS
PHOTOSPHERE
SOLAR ATMOSPHERE
SPECTRA
WAVE PROPAGATION