Theoretical correlations between prominence plasma parameters and the emitted radiation

Details Theoretical correlations between prominence plasma parameters and the emitted radiation Theoretical correlations between prominence plasma parameters and the emitted radiation

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..656h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 2, p. 656-668

Computer Science

Numerical Analysis

40

Computerized Simulation, Correlation, H Alpha Line, Hydrogen, Radiation, Solar Prominences, Stellar Models, Balmer Series, Lyman Spectra, Numerical Analysis

Scientific paper

Recently a set of 140 prominence non-local thermodynamic equilibrium (NLTE) models has been computed using the best available numerical techniques (Gouttebroze et al. 1993, hereafter GHV). Models are represented by one-dimensional (1D) slabs vertically standing on the solar surface and irradiated by photospheric and chromospheric radiation. They are parameterized by the gas pressure and temperature (uniform), the geometrical thickness of the 1D slab, the microturbulent velocity and the height above the solar surface. As outputs we obatined several physical quantities and optical parameters like the electron density, the total hydrogen density, the optical thickness in hydrogen lines and continua, spectral line intensities etc. (see GHV). In order to establish mutual correlations between various plasma parameters and the basic characteristics of the synthesized hydrogen spectrum, we construct some basic correlation curves. A very important relation already mentioned in GHV concerns the plasma emission measure found to be closely related to the integrated intensity of the Balmer H-alpha line. We present several other correlations which can be divided into four categories: (1) relations between radiation properties themselves; (2) radiation properties versus plasma parameters; (3) the H-alpha source function behavior; and (4) correlations between plasma parameters. Together with the 24 presented figures, we discuss the physical interpretation of these correlations and we give some hints for their application to the observed data. When appropriate, we also compare our results with existing observations.

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