The formation of helioseismology lines. IV - The NI I 676.8 NM intercombination line

Details The formation of helioseismology lines. IV - The NI I 676.8 NM intercombination line The formation of helioseismology lines. IV - The NI I 676.8 NM intercombination line

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...269..509b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 269, no. 1-2, p. 509-517.

Astronomy and Astrophysics

Astrophysics

24

Helioseismology, Line Spectra, Metallicity, Nickel, Line Shape, Photosphere, Solar Granulation

Scientific paper

The Ni I 676.8 nm intercombination line will be used as velocity diagnostic in helioseismology with the instruments of the Global Oscillations Network Group and the Michelson Doppler Imager onboard SOHO. In this analysis, I employ the VAL3-C plane-parallel model of the quiet solar atmosphere and a snapshot of a Nordlund and Stein solar granulation simulation as input for studying the NLTE behavior and the sensitivity to granulation of this line. The nickel atom is ironlike in its structure and complexity, but more regular and easier to model. The NLTE mechanisms involved are ultraviolet overionization, infrared overrecombination, optical line pumping, and line photon losses. I assess their relative importance and the effects imposed by the solar granulation and confirm that the line is a good choice for helioseismology.

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