Physical conditions in the cool parts of spicules

Details Physical conditions in the cool parts of spicules Physical conditions in the cool parts of spicules

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...284..833l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 284, Sept. 15, 1984, p. 833-838.

Physics

10

Chromosphere, Solar Atmosphere, Solar Physics, Solar Spectra, H Lines, Plasma Turbulence, Resonance Lines, Spicules

Scientific paper

The resonance lines of Na, Sr(+), and the Mg triplet system, together with the middle H Balmer lines, are used to determine the plasma parameters in the cool parts of spicules. Results are presented for the heights 2100 and 2500 km according to the chromospheric line emission data reported by Dunn et al. (1968) for the 1962 eclipse. The low flow-velocity solutions require unsatisfactorily high temperature and microturbulence values (the derived thicknesses are also uncomfortably large). The remaining solutions have flow velocities and thicknesses that are in line with expectations from direct spicule observations, and the electron densities are comparable to those obtained from continuum measurements at the 1952 eclipse. However, contrary to most preconceptions, hydrogen is found to be predominantly neutral in these regions; the total gas pressure is consequently quite large - in fact, exceeding the adjacent interspicular pressure by about a factor of 10.

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