Observations of the Profiles of Solar UV Emission Lines and Their Analysis in Terms of the Heating and Production of the Corona

Details Observations of the Profiles of Solar UV Emission Lines and Their Analysis in Terms of the Heating and Production of the Corona Observations of the Profiles of Solar UV Emission Lines and Their Analysis in Terms of the Heating and Production of the Corona

Sep 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ssrv...13..639b&link_type=abstract

Ultraviolet and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, Proceedinsg of IAU Colloq. 14, held in Utrecht, Augu

Astronomy and Astrophysics

Astrophysics

Scientific paper

Observations of the solar spectrum have been made between 1200 2200 Å with high spectral resolution. The results were obtained with an all-reflecting echelle spectrograph carried by a stabilized Skylark rocket launched in April 1970. Measurements of the profiles of a number of emission lines due to Si ii, C ii, Si iii and C iv formed in the temperature range 104-105 K, indicate ion energies which are considerably in excess of the electron temperatures derived from the ionization balance. Since the ion/electron relaxation time is very short the observed ion energies cannot correspond to an ion temperature and hence a non-thermal mechanical energy component exists in the transition zone. It is postulated that the non-thermal energy component represents the actual mechanical energy responsible for the heating of the corona, and, that, it is propagated as an acoustic wave. On this basis and with a preliminary estimate of the reflection from the transition zone, a flux of 3 × 105 erg cm -2 s -1 is established as entering the corona. This value is in agreement with estimates of the total energy loss from the corona due to conduction, radiation and the solar wind, thus establishing a gross energy balance. Theoretical calculations are currently underway to establish the physical nature of the atmosphere which would result from such a propagating flux. At the present time this has been carried out for an atmosphere in hydrostatic equilibrium and the energy balance equation solved. A preliminary temperature structure which results is shown in Figure 1, together with the derived distribution in electron density. This gives a corona of the right temperature and density but the observed structure deviates in detail from those derived from an analysis of the solar XUV spectrum.

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