The brightening of sunspot umbra observed on 29 October, 1972

Details The brightening of sunspot umbra observed on 29 October, 1972 The brightening of sunspot umbra observed on 29 October, 1972

Oct 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...38..389k&link_type=abstract

Solar Physics, vol. 38, Oct. 1974, p. 389-398.

Physics

4

Luminous Intensity, Mass Flow, Solar Corona, Solar Prominences, Sunspots, Umbras, Brightness, Kinetic Energy, Line Spectra, Solar Spectra, Spectral Line Width, Spectroheliographs

Scientific paper

Brief descriptions are given of the spectroscopic and the monochromatic observations of the umbral brightening on Oct. 29, 1972. The source of the brightening is attributed to the kinetic energy of the infalling coronal matter with a final velocity of 200 km per sec, into the umbral gas. The spectra of this brightening reveal many hydrogen and metallic emission lines. The variety of the widths of these lines indicates the existence of complex nonthermal velocity field and of the stratification of various emitting conditions in the umbral brightening. The kinetic energy of the falling matter would be expended not only for producing the emissions, but also for exciting the complex velocity field of nonthermal motion.

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