Use of Al xii and Mg xi lines as solar plasma diagnostics |
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| Authors: | B J I Bromage K J H Phillips F P Keenan S M McCann |
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| Institution: | (1) Astrophysics Division, Rutherford Appleton Laboratory, OX 11 0QX Chilian, Didcot, Oxfordshire, U.K.;(2) Department of Pure and Applied Physics, Queen's University, BT7 1NN Belfast, Northern Ireland |
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| Abstract: | We present three sets of observations of n = 1 to n = 2 lines due to helium-like aluminium (Alxii), made during two solar flares (25 August, 1980 and 19 October, 1986), using the X-Ray Polychromator on the SMM satellite. The observed temperature-sensitive line ratio G is shown to be consistent with the close-coupling calculations of Keenan and McCann (1987), although the ratio R, which is both temperature and density-sensitive for lower-Z elements, is not sufficiently well determined from these data to say more than that the observed values of R are not inconsistent with the theoretical calculations. This region of the spectrum also includes the helium-like magnesium (Mgxi) 11
S - 31
P line, and it is shown that the ratio of this line to the Alxii resonance (11
S - 21
P) line is a more sensitive indicator of electron temperature than are the Alxii
G and R ratios. We demonstrate that the three ratios may be used together in order to derive values of emission measure, electron temperature and electron density during these flares. |
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