Fe XVII X-ray lines in solar coronal plasmas

Details Fe XVII X-ray lines in solar coronal plasmas Fe XVII X-ray lines in solar coronal plasmas

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..20.2267p&link_type=abstract

Advances in Space Research, Volume 20, Issue 12, p. 2267-2270.

Computer Science

Scientific paper

Calculated intensities of the Fe xvii X-ray lines due to transitions 2p^6 - 2p^53d lines (near 15 A˚) and 2p^6 - 2p^53s lines (near 17 A˚) are compared with measured line intensities in solar and tokamak spectra. For the solar spectra, temperature T_e is obtained from the ratio of the Fe xvii 16.776 A˚ line to a nearby Fe xviii line. We find excellent agreement for all the major Fe xvii line features in the 15-17 A˚ region except the Fe xvii 15.015 A˚ line, the observed flux of which is less than the theoretical by a factor f. We find that f strongly depends on the heliocentric angle theta of the emitting region, being smallest (0.2) when the region is nearest Sun centre, but nearly 1 near the limb. Attributing this to resonance scattering, we are able to deduce the path length and electron density from the observations. Possible application to stellar active regions is given.

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