Diamagnetic propulsion and energy balance of magnetic elements in the solar chromosphere and transition region

1984 ◽  
Vol 276 ◽  
pp. 369 ◽  
Author(s):  
P. J. Cargill ◽  
G. W. Pneuman
Keyword(s):  
Energy Balance ◽  
Transition Region ◽  
Solar Chromosphere ◽  
Magnetic Elements

Effects of Ambipolar Diffusion on Prominence Thread Models

1994 ◽  
Vol 144 ◽  
pp. 315-321 ◽  
Author(s):  
M. G. Rovira ◽  
J. M. Fontenla ◽  
J.-C. Vial ◽  
P. Gouttebroze
Keyword(s):  
Energy Balance ◽  
Transition Region ◽  
Ambipolar Diffusion ◽  
Line Profiles ◽  
Balance Equations ◽  
Model Calculations ◽  
Partial Frequency ◽  
Frequency Redistribution ◽  
Partial Frequency Redistribution ◽  
Theoretical Structure

AbstractWe have improved previous model calculations of the prominence-corona transition region including the effect of the ambipolar diffusion in the statistical equilibrium and energy balance equations. We show its influence on the different parameters that characterize the resulting prominence theoretical structure. We take into account the effect of the partial frequency redistribution (PRD) in the line profiles and total intensities calculations.

High-resolution, far-ultraviolet study of Beta Draconis (G2 Ib-II) - Transition region structure and energy balance

1984 ◽  
Vol 283 ◽  
pp. 731 ◽  
Author(s):  
A. Brown ◽  
C. Jordan ◽  
R. E. Stencel ◽  
J. L. Linsky ◽  
T. R. Ayres
Keyword(s):  
Energy Balance ◽  
High Resolution ◽  
Transition Region ◽  
Far Ultraviolet

scholarly journals Energy Balance in Prominence-Corona Transition Regions

1990 ◽  
Vol 142 ◽  
pp. 325-329
Author(s):  
C. Chiuderi ◽  
F. Chiuderi Drago
Keyword(s):  
Energy Balance ◽  
Transition Region ◽  
Coronal Plasma

Prominences are sheets of cold (< 104 K) plasma totally imbedded in the hot (> 106 K) coronal plasma. A Prominence-Corona Transition Region (PCTR) is therefore present all around it.

scholarly journals Experiment to Determine the Temperature Structure in the Solar Chromosphere and Corona

1972 ◽  
Vol 14 ◽  
pp. 668-669
Author(s):  
C. R. Negus
Keyword(s):  
Transition Region ◽  
Extreme Ultraviolet ◽  
Normal Incidence ◽  
Research Unit ◽  
Emission Lines ◽  
Solar Chromosphere ◽  
Temperature Structure ◽  
Ultraviolet Emission ◽  
Ionization Temperature ◽  
Intensity Ratios

An experiment is in course of preparation at the Astrophysics Research Unit at Culham for flight on a Sun-pointing rocket. It is designed to determine the ionization temperature and electron density as a function of height in the temperature range of about 8 × 104 K to 3 × 106 K by measuring limb to disk intensity ratios of extreme ultraviolet emission lines in the 170 to 850 Å region. The work is an extension of current experiments in which normal-incidence spectrographs are used to determine the structure lower in the chromosphere-corona transition region.

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