HRTS II EUV observations of a solar ephemeral region

Details HRTS II EUV observations of a solar ephemeral region HRTS II EUV observations of a solar ephemeral region

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...278..428r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 278, March 1, 1984, p. 428-440.

Astronomy and Astrophysics

Astrophysics

5

Chromosphere, Extreme Ultraviolet Radiation, High Resolution, Solar Magnetic Field, Stellar Spectrophotometry, Emission Spectra, Line Spectra, Solar Corona, Solar Spectra, Solar Temperature, Solar Wind, Spectrographs, Telescopes, Ultraviolet Spectra

Scientific paper

HRTS II has been used to observe the EUV emission of a small bipolar magnetic feature or ephemeral region, where strong EUV line enhancement exhibits contrasts (measured relative to the quiet sun) which range from 10 to 70. The substantiality of the Lyman-alpha and C II-O V emission, and the absence of any measurable emission in coronal forbidden lines, sets a temperature range for the loop's active part of the order of 16,000-300,000 K. The use of the ratios of allowed lines as temperature diagnostics yields temperatures that are very near ionization equilibrium temperatures, and the use of chromospheric lines to form a wavelength standard yields absolute velocities ranging in magnitude from zero to 12 km/sec for C IV, N IV, and O V. This flow is interpreted as a siphon flow.

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