The Relative Abundance of Neon and Magnesium in the Solar Corona.

摘要

A technique is proposed 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 NeX (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. Relatively low 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.