Dynamics of solar filaments. III - Analysis of steady flows in H-alpha and C IV lines

Details Dynamics of solar filaments. III - Analysis of steady flows in H-alpha and C IV lines Dynamics of solar filaments. III - Analysis of steady flows in H-alpha and C IV lines

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...136...81s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 136, no. 1, July 1984, p. 81-88.

Astronomy and Astrophysics

Astrophysics

26

Chromosphere, Faculae, Solar Prominences, Solar Spectra, H Alpha Line, Magnetohydrodynamic Flow, Radial Velocity, Radiant Flux Density, Solar Atmosphere, Solar Corona, Solar Velocity

Scientific paper

A statistical analysis of intensities and radial velocities of several solar plage filaments (i.e. prominences seen on the solar disk) observed at disk center is presented. Intensity and radial (= vertical) velocity maps were derived from simultaneous 2D measurements of the H-alpha chromospheric line with the Multichannel Subtractive Double Pass spectrograph operating on the Meudon solar tower, and also obtained from 2D recordings of the C IV transition-zone line (1548 A) with the UV Spectrometer and Polarimeter aboard the Solar Maximum Mission satellite. A good correlation (around 0.5) is found between intensities in both lines, as well as between velocities. Persistent upflows are measured in both lines at the filament location. The mean vertical velocities are respectively 0.5 km/s in H-alpha and 5.6 km/s in C IV. The analysis of mass fluxes suggests that C IV upflows occur in the transition region around prominences rather than below, in the chromosphere-corona transition zone.

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