A Comparison of Theoretical mgvi Emission Line Strengths with Active-Region Observations From Serts |
| |
| Authors: | F.P. Keenan M. Mathioudakis A.C. Katsiyannis C.A. Ramsbottom K.L. Bell R.J. Thomas J.W. Brosius |
| |
| Affiliation: | (1) Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, BT7 1NN, Northern Ireland;(2) Department of Applied Mathematics and Theoretical Physics, The Queen's, University of Belfast, Belfast, BT7 1NN, Northern Ireland;(3) Laboratory for Astronomy and Solar Physics, Code 682, NASA Goddard Space Flight Center, Greenbelt, MD, 20771, U.S.A;(4) Raytheon ITSS, 4400 Forbes Boulevard, Lanham, MD 20706, U.S.A |
| |
| Abstract: | R-matrix calculations of electron impact excitation rates in N-like Mg vi are used to derive theoretical electron-density-sensitive emission line ratios involving 2s22p3–2s2p4transitions in the 269–403 Å wavelength range. A comparison of these with observations of a solar active region, obtained during the 1989 flight of the Solar EUV Rocket Telescope and Spectrograph (SERTS), reveals good agreement between theory and observation for the 2s22p34S–2s2p44Ptransitions at 399.28, 400.67, and 403.30 Å, and the 2s22p32P–2s2p42Dlines at 387.77 and 387.97 Å. However, intensities for the other lines attributed to Mgvi in this spectrum by various authors do not match the present theoretical predictions. We argue that these discrepancies are not due to errors in the adopted atomic data, as previously suggested, but rather to observational uncertainties or mis-identifications. Some of the features previously identified as Mgvi lines in the SERTS spectrum, such as 291.36 and 293.15 Å, are judged to be noise, while others (including 349.16 Å) appear to be blended. |
| |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ |
|
