Abstract
This is a quantitative investigation of the electron beam effect on the hydrogen line profiles and continuum intensity distribution during the impulsive phase of flares. The flaring atmosphere is suggested to be a hydrogenic one and its physical condition corresponds to the gas dynamics problem solution. The radiative transfer, steady-state and particle conservation equations are solved for the three-level hydrogen model atoms with continua. Return-current losses were neglected. Hydrogen line profiles are found to be slightly sensitive to nonthermal impacts with beam electrons in the cores and more sensitive in the wings. With the initial energy flux,F 0, rising and energy spectral index, δ, decreasing, the wing intensities begin to increase, and the Hα lines are shown to have rather extended wings as is often observed. The hydrogen continua are shown to be strongly affected by nonthermal impacts. The bigger the value ofF 0 and the smaller the value of δ, the greater absolute intensities of the hydrogen continua heads. This effect is more noticeable for the Balmer and Paschen continua. The head intensity slopes of them can be used for determination of these electron beam parameters on depths of the hydrogen emission origin and their following comparison with the same parameters for the coronal heights from the X-ray observations.
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References
Aboudarham, J. and Hénoux, J.-C.: 1986a,Adv. Space Res. 6, 131.
Aboudarham, J. and Hénoux, J.-C.: 1986b,Astron. Astrophys. 168, 301.
Brown, J. C.: 1971,Solar Phys. 18, 489.
Burgess, A.: 1964,Mem. Roy. Astron. Soc. 69, 1.
Cheng, C.-C. and Pallavicini, R.: 1988,Astrophys. J. 324, 1138.
Cheng, C.-C., Orwig, L. E., and Tandberg-Hanssen, E.: 1987,Solar Phys. 113, 301.
Emslie, A. G.: 1978,Astrophys. J. 224, 241.
Hiei, E.: 1987,Solar Phys. 113, 249.
Hudson, H. S.: 1972,Solar Phys. 24, 414.
Johnson, L. C.: 1972,Astrophys. J. 174, 227.
Kurokawa, H., Takakura, J., and Ohki, H.: 1988,Publ. Astron. Soc. Japan 40, 357.
Lin, R. P. and Hudson, H. S.: 1976,Solar Phys. 50, 153.
Machado, M. E., Avrett, E. H., Vernazza, J. E., and Noyes, R. W.: 1980,Astrophys. J. 242, 336.
Neidig, D. F. and Wiborg, P. H.: 1984,Solar Phys. 92, 217.
Ricchiazzi, P. J. and Canfield, R. G.: 1983,Astrophys. J. 272, 739.
Somov, B. V.: 1987,Results Sci. Tech., Ser. Astron. (USSR) 34, 78.
Somov, B. V., Spektor, A. R., and Syrovatskii, S. I.: 1981,Solar Phys. 73, 145.
Syrovatskii, S. I. and Shmeleva, O. P.: 1972,Astron. Zh. 49, 334.
Zharkova, V. V.: 1990,Kiev University News Report, Ser. Astronomy 31, 47.
Zharkova, V. V. and Kobylinsky, V. A.: 1989,Letter Astron. J. (USSR) 15, 847.
Zharkova, V. V. and Kobylinsky, V. A.: 1991,Letter Astron. J. (USSR) 17, 75.
Zharkova, V. V. and Kobylinsky, V. A.: 1992,Kinematics Phys. Celest. Bodies 8, No. 3, 38.
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Zharkova, V.V., Kobylinsky, V.A. The effect of non-thermal excitation and ionization on the hydrogen emission in impulsive solar flares. Sol Phys 143, 259–274 (1993). https://doi.org/10.1007/BF00646487
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DOI: https://doi.org/10.1007/BF00646487