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Stationary equations of hydrogen excitation and ionization in prominences

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Abstract

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 Hα line has attained 56 mÅ of the disc centre spectrum) is completely due to scattering of the Sun radiation. The basic unknowns are separated with certainty: electron concentration (n e = 3.0 × 1010 cm−3), effective thickness (l = 4.2 × 108 cm) and electron temperature (T e = 5000 K).

Radiation of a very bright prominence (A λ(Hα) = 213 mÅ; T e = 7300 K; n e = 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.

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References

  • Baker, J. and Menzel, D.: 1938, Astrophys. J. 88, 52.

    Google Scholar 

  • Ivanov, V. V.: 1969, Radiative Transfer and Heavenly Body Spectra, ‘Nauka’, Moscow.

    Google Scholar 

  • Jager, C. de: 1952, Rech. Astron. Observ. Utrecht, XIII, part I.

  • Kingston, A. E.: 1964, Astrophys. J. 140, 736.

    Google Scholar 

  • Kuli-Zade, D. M.: 1964, Astron. Zh. 41, 920.

    Google Scholar 

  • Matsushima, S.: 1952, Astrophys. J. 115, 544.

    Google Scholar 

  • Polupan, P. N. and Yakovkin, N. A.: 1965, Astron. Zh. 42, 764.

    Google Scholar 

  • Sampson, D. H. and Golden, L. B.: 1970, Astrophys. J. 161, 321.

    Google Scholar 

  • Sobolev, V. V.: 1962, Astron. Zh. 39, 632.

    Google Scholar 

  • Sobolev, V. M.: 1961, Bull. Pulkovo Obs. No. 167, 52.

  • Thomas, R. N. and Athay, R. G.: 1961, Physics of the Solar Chromosphere, Interscience Publishers Ltd., London.

    Google Scholar 

  • Wiese, W. Z., Smith, M. W., and Glennon, B. M.: 1966, Atomic Transition Probabilities I, Institute for Basic Standards National Bureau of Standards, Washington D.C.

    Google Scholar 

  • Yakovkin, N. A. and Zeldina, M. Yu.: 1963, Astron. Zh. 40, 847.

    Google Scholar 

  • Yakovkin, N. A. and Zeldina, M. Yu.: 1964, Soln. Dann. Bull. No. 9, 62.

  • Yakovkin, N. A. and Zeldina, M. Yu.: 1968, Astron. Zh. 45, 50.

    Google Scholar 

  • Yakovkin, N. A. and Zeldina, M. Yu.: 1969, Vest. Kiev. Univ. Ser. Astron. No. 11, 18; 1971, No. 13, 31.

  • Yeh Shih-Huei: 1961, Izv. Krymsk. Astrofiz. Obs. 25, 180.

    Google Scholar 

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Authors and Affiliations

  1. Astronomical Observatory, Ulan-Bator, M.P.R.

    Ts. Chultem

  2. Kiev University Observatory, Kiev, U.S.S.R.

    N. A. Yakovkin

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  1. Ts. Chultem
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  2. N. A. Yakovkin
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Chultem, T., Yakovkin, N.A. Stationary equations of hydrogen excitation and ionization in prominences. Sol Phys 34, 133–150 (1974). https://doi.org/10.1007/BF00149605

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