Emission features in the solar corona after the perihelion passage of Comet 1979 XI

Details Emission features in the solar corona after the perihelion passage of Comet 1979 XI Emission features in the solar corona after the perihelion passage of Comet 1979 XI

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..91...71c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 91, no. 1, March 1983, p. 71-77.

Astronomy and Astrophysics

Astrophysics

6

Abundance, Astronomical Photography, Comets, Emission Spectra, Solar Corona, Coronagraphs, Cosmic Dust, Iron, Nickel, Silicon, Solar Limb, Spectroheliographs

Scientific paper

On the coronograph spectrophotographic records taken on 31.372 UT, August 1979, some faint emission features were found which can be ascribed to Si II and Ni II. These emissions were obviously a transient phenomena which were detected only 10 hr after the supposed fall of Comet 1979 XI in the Sun's photosphere. It cannot be excluded that the appearance of Si and Ni lines was triggered by the evaporation of dust particles with a high abundance of heavier elements in the solar corona. This assumption is also supported by the intensity distribution of the Fe X coronal line around the Sun's limb. The maximum coincides with the position angle of the projected path of the comet.

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