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Dynamics of the solar transition zoneTime-resolved profiles of the 1548-A C IV line arising from the solar transition region are analyzed in order to determine whether the 300-sec oscillations characteristic of the photosphere and chromosphere penetrate into the transition zone and to measure the rms amplitude of transition-zone disturbances as well as their dependence on solar activity. The rms velocity amplitude is used to set limits on the mechanical energy flux available for solar heating. A power-spectrum analysis indicates that acoustic waves appear to have been detected in the transition zone, that at least one case of a strong 200- to 300-sec oscillation was observed, but that strong periodicities are not found on the average in either the intensity or the velocity field. It is suggested that the rms velocity that may be attributed to directly observable wave motion is between 3 and 7 km/s, depending on whether the individual emission elements seen in rocket spectra are coherent or independent in phase.
Document ID
Document Type
Reprint (Version printed in journal)
External Source(s)
Bruner, E. C., Jr.
(Lockheed Research Laboratories Palo Alto, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
December 15, 1978
Publication Information
Publication: Astrophysical Journal
Subject Category
Solar Physics
Funding Number(s)
Distribution Limits
No Preview Available