The Temperature Structure, Mass, and Energy Flow in the Corona and Inner Solar Wind (original) (raw)
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Abstract
Data from remote-sensing and in situ instruments are used as empirical constraints on a radiative energy balance model in order to determine the radial variations of coronal temperatures, densities, and outflow speeds in several types of coronal holes and a quiet, unstructured region of the corona. The one-fluid solar wind model used in the investigation includes the effects of radiative and inward conductive losses in the low corona and the chromospheric-coronal transition region. It satisfactorily accounts for a variety of measurements of coronal and solar wind parameters for an equatorial coronal hole, polar coronal holes at solar minimum and solar maximum, and an unstructured quiet region of the corona.
Publication:
The Astrophysical Journal
Pub Date:
February 1988
DOI:
Bibcode:
Keywords:
- Plasma Temperature;
- Solar Corona;
- Solar Wind;
- Coronal Holes;
- Energy Transfer;
- Extreme Ultraviolet Radiation;
- Magnetohydrodynamic Waves;
- Mass Distribution;
- Plasma Density;
- Solar Physics;
- SUN: CORONA;
- SUN: SOLAR WIND