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X-ray Lines From Mg VIII and Si X Ions and Their Diagnostic Use

Published online by Cambridge University Press:  12 April 2016

Bhola N. Dwivedi
Bhola N. Dwivedi*
Affiliation:
Department of Applied Physics, Institute of Technology, Banaras Hindu University, Varanasi-221 005, India

Abstract

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The solar X-ray emission lines from Mg VIII and Si X ions have been studied. The variation of theoretical line intensity ratio I(λ 75.03)/I(λ 74.86) from Mg VIII and I(λ 50.69)/I(λ 50.52) from Si X as a function of electron density is found to be good density monitors of the emitting regions of solar plasma. The computed values of line intensity from these ions based on Kopp and Orrall model have been used to derive electron density of the quiet Sun and coronal holes. The electron densities of 109 cm-3 and 4.6 × 108 cm-3 are estimated at the electron temperatures of 8 x 105 K and 1.6 x 106 K for the quiet Sun whereas the respective values of 5.4 x 108 cm-3 and 1.7 x 108 cm-3 are obtained for the coronal holes. The line intensity ratios studied here are independent of temperature variation and are therefore excellent candidates for electron density diagnostics. However, observational data with improved spectral resolution is needed for using X-ray line pairs studied for their diagnostic use.

Type
1. X-rays from a Hot Plasma
Information
International Astronomical Union Colloquium , Volume 115: High Resolution X-ray Spectroscopy of Cosmic Plasmas , 1990 , pp. 40 - 43
Copyright
Copyright © Cambridge University Press 1990

References

Brown, W.A., Bruner, M.E., Acton, L.W., and Mason, H.E. 1986, Ap. J., 301, 981.Google Scholar
Dwivedi, B.N. and Raju, P.K., 1980, Solar Phys., 68, 111.Google Scholar
Dwivedi, B.N. 1988, Solar Phys. Lett., in pressGoogle Scholar
Elwert, G. and Raju, P.K. 1975, Ap. Space Sci., 38, 369.Google Scholar
Elzner, L.R. 1976, Astr. Ap., 47, 9.Google Scholar
Flower, D.R. and Nussbaumer, H. 1975a, Astr. Ap., 45, 145.Google Scholar
Flower, D.R. and Nussbaumer, H. 1975b, Astr. Ap., 45, 349 Google Scholar
Jordan, C. 1969, M.N.R.A.S., 142, 501.Google Scholar
Kopp, R.A. and Orrall, F.Q. 1976, Astr. Ap., 53, 363.Google Scholar
Malinovsky, M. and Heroux, L. 1973, Ap. J., 226, 720.Google Scholar
Saha, H.P. and Trefftz, E. 1983, Solar Phys., 87, 720 Google Scholar
Vernazza, J.E. and Mason, H.E. 1978, Ap. J., 226, 720.Google Scholar