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Astron. Astrophys. 325, 803-812


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Emission of hydrogen lines by moving solar prominences

C. Gontikakis, J.-C. Vial, and P. Gouttebroze

Institut d'Astrophysique Spatiale, Unité mixte CNRS-Université Paris XI, Bâtiment 121, F-91405 Orsay Cedex, France

Received 19 November 1996 / Accepted 24 March 1997

Abstract

We study the radiative transfer processes occurring in a plane-parallel slab standing vertically above the chromosphere and moving upward as a solid body. This structure simulates a prominence in the phase of eruption or a quiescent prominence where the plasma presents bulk velocities. We use partial redistribution for the description of the resonance scattering in the hydrogen L FORMULA and L FORMULA lines. We compute the L FORMULA , L FORMULA and H FORMULA emergent line profiles of hydrogen for different velocities. We derive the variation of the emitted intensities as a function of the velocity for various temperatures and thicknesses. We discuss our results in view of the diagnostic of erupting prominences in Lyman lines that SOHO observations can provide.

Key words: radiative transfer - prominences - radial velocities

Send offprint requests to: J.-C. Vial


© European Southern Observatory (ESO) 1997

Online publication: September 9, 1997
Last change: April 28, 1998
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