Laboratory Measurements of the Fe XVII 2p-3s and 2p-3d Transitions and Comparison with Solar and Astrophysical Observations

Details Laboratory Measurements of the Fe XVII 2p-3s and 2p-3d Transitions and Comparison with Solar and Astrophysical Observations Laboratory Measurements of the Fe XVII 2p-3s and 2p-3d Transitions and Comparison with Solar and Astrophysical Observations

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...610..616b&link_type=abstract

The Astrophysical Journal, Volume 610, Issue 1, pp. 616-623.

Astronomy and Astrophysics

Astronomy

20

Atomic Processes, Galaxies: Individual: Ngc Number: Ngc 4636, Line: Formation, Stars: Coronae, Stars: Individual: Name: Capella, Stars: Individual: Constellation Name: Ii Pegasi, Stars: Individual: Name: Procyon, Stars: Individual: Constellation Name: Yy Geminorum, Sun: X-Rays, Gamma Rays

Scientific paper

The L-shell emission spectrum of Fe XVII is measured in high-temperature laboratory plasmas, and the inferred intensities of the 3s-->2p transitions relative to those of the dominant 3d-->2p transition are compared to solar observations, as well as to observations of Capella, Procyon, Castor C, II Pegassi, and NGC 4636 with the Chandra and XMM-Newton X-ray observatories. The results from laboratory and astrophysical plasmas are in very good agreement, indicating that the collisional line formation processes found in low-density, high-temperature laboratory plasmas are a good description of those found in astrophysical plasmas. The laboratory observations disagree, however, to varying degrees with spectral modeling calculations. A review of existing laboratory measurements suggests that the intensity of the dominant 3d-->2p transition is overestimated by spectral modeling predications. By calibrating spectral models with laboratory data, especially by decreasing the strength of the dominant 3d-->2p transition, spectral models can be brought into agreement with the majority of solar and astrophysical observations. Without doing so, opacity effects may be grossly overestimated.

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