The relative abundance of neon and magnesium in the solar corona

Details The relative abundance of neon and magnesium in the solar corona The relative abundance of neon and magnesium in the solar corona

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...203l.139r&link_type=abstract

Astrophysical Journal, vol. 203, Feb. 1, 1976, pt. 2, p. L139-L143.

Astronomy and Astrophysics

Astrophysics

10

Abundance, Magnesium, Neon, Solar Corona, Solar Spectra, Atomic Spectra, Line Spectra, Luminous Intensity, Ultraviolet Spectra

Scientific paper

A relationship between the calculated emission functions for Ne X and Mg XI is discussed and used for determining the relative solar coronal abundance of neon and magnesium. The relative abundance is calculated directly from the relative intensity of the resonance lines of Ne X(12.134 A) and Mg XI (9.169 A) without the need for the development of a detailed model of the thermal structure of the corona. Moderate-resolution Bragg-crystal spectrometer results from the OV1-10 satellite are used to determine a coronal neon to magnesium relative abundance of 1.47 plus or minus 0.38. The application of this technique to a recent higher-resolution rocket observation gives an abundance ratio of approximately 0.93 plus or minus 0.15.

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