On the Rate of Abundance Modifications versus Time in Active Region Plasmas

Details On the Rate of Abundance Modifications versus Time in Active Region Plasmas On the Rate of Abundance Modifications versus Time in Active Region Plasmas

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...555..426w&link_type=abstract

The Astrophysical Journal, Volume 555, Issue 1, pp. 426-434.

Astronomy and Astrophysics

Astronomy

34

Sun: Abundances, Sun: Activity, Sun: Corona

Scientific paper

Four emerging and developing active regions observed on Skylab spectroheliograms (300-600 Å) have been studied over intervals of 3 to 7 days to determine the change in their Mg/Ne abundance ratio. The Mg/Ne abundance ratio is used as a measure of the FIP effect on element abundances in the solar upper atmosphere. Mg/Ne abundance ratios were derived from diagnostic intensity ratios of Mg VI lines at 400 Å relative to adjacent Ne VI lines. Intensity ratios were estimated from the active region images in the Skylab Atlas of Extreme-Ultraviolet Spectroheliograms. The resulting abundance ratios expressed in terms of the FIP bias β (see text) are plotted as a function of elapsed time since emergence. After emergence the newborn region shows photospheric composition: i.e., the abundance ratio of Mg/Ne=0.296, β=1. Thereafter, the developing regions show a progressive increase in the Mg/Ne abundance ratio with the value of β reaching after 2 days coronal-type abundances: Mg/Ne=1.43, β~4.8. In the later stages, the bias increases to values between 7 and 9 after 3 to 7 days. Some implications of the abundance modifications are briefly discussed.

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