The relative abundance of neon and magnesium in the solar corona | Zendy

H. R. Rugge | Zendy; Jr. Walker A. B. C. | Zendy

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The relative abundance of neon and magnesium in the solar corona

Author(s) -

H. R. Rugge,

Jr. Walker A. B. C.

Publication year - 1976

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/182038

Subject(s) - neon , physics , spectral line , astrophysics , solar radius , magnesium , emission spectrum , astronomy , solar wind , atomic physics , plasma , coronal mass ejection , chemistry , argon , nuclear physics , organic chemistry

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 +- 0.38. The application of this technique to a recent higher resolution rocket observation gives an abundance ratio of approx.0.93 +- 0.15. (AIP)

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