Stationary equations of hydrogen excitation and ionization in prominences

✍ Scribed by Ts. Chultem; N. A. Yakovkin

• Publisher: Springer
• Year: 1974
• Tongue: English
• Weight: 773 KB
• Volume: 34
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00149605

✦ Synopsis

The statistical equilibrium equations for the continuum and first 10 levels of a hydrogen atom show that the radiation of a bright prominence (the brightness of the H~ line has attained 56 m/k of the disc centre spectrum) is completely due to scattering of the Sun radiation. The basic unknowns are separated with certainty: electron concentration (ne=3.0• 101~ effective thickness (l = 4.2 • 108 cm) and electron temperature (Te = 5000 K).

Radiation of a very bright prominence (Az(Ha) --213 rn~; Te=7300 K; ne = 5.0 • 1011 cm-3; l= 1.3 • 107 cm) is on account of electron impacts (40%) and the Sun radiation scattering (60%).

The parameters are shown to depend greatly on the prominence optical thickness in the lines of the first subordinate series of a hydrogen atom. In the course of determination all the parameters and 100 interconnected integral equations of the radiation diffusion have been thickness-averaged; the population of levels has been calculated by observations using the self-absorption factors.