Abstract
A technique for analyzing measurements of XUV spectral line intensities is described. Application of the technique to OSO-4 and OSO-6 spectra indicates that the mean coronal temperature is 2.1 × 106 K in typical active solar regions and that the mean coronal temperature in typical quiet regions ranges from 1.5 × 106 to 2.1 × 106 K. One active region spectrum shows evidence for substantial quantities of coronal material with 2 × 106 < T < 3.5 × 106 K. Measurements from limb spectra show evidence that (1) coronal abundances of N and O are low relative to heavier elements; or (2) that the ionization equilibrium calculations used may contain systematic errors; or (3) that the XUV intensity measurements may be incorrectly calibrated.
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References
Allen, J. W. and Dupree, A. K.: 1969, Astrophys. J. 155, 27.
Athay, R. G.: 1966, Astrophys. J. 145, 784.
Bely, O.: 1966, Proc. Phys. Soc. 88, 587.
Delache, P.: 1967, Ann. Astrophys. 30, 827.
Dupree, A. K.: 1972, Astrophys. J. 178, 527.
Dupree, A. K. and Goldberg, L.: 1967, Solar Phys. 1, 229.
Dupree, A. K. and Reeves, E. M.: 1971 Astrophys. J. 165, 599.
Dupree, A. K., and Wood, A. T.: 1969, personal communication.
Dupree, A. K., Huber, M. C. E., Noyes, R. W., Parkinson, W. H., Reeves, E. M., and Withbroe, G. L.: 1973, Astrophys. J. 182, 331
Foukal, P. V.: 1975, Solar Phys., 43, 327.
Jefferies, J. T., Orrall, F. Q., and Zirker, J. B.: 1972, Solar Phys. 22, 307.
Jordan, C.: 1969, Monthly Notices Roy. Astron. Soc. 142, 501.
Jordan, C. and Pottasch, S. R.: 1968, Solar Phys. 4, 104.
Kopp, R. A.: 1972, Solar Phys. 27, 373.
Malinovsky, M. and Heroux, L.: 1973, Astrophys. J. 181, 1009.
Mariska, J. T. and Withbroe, G. L.: 1975, Solar Phys., in press.
Pottasch, S. R.: 1964, Space Sci. Rev. 3, 816.
Pottasch, S. R.: 1967, Bull. Astron. Inst. Neth. 19, 113.
Reimers, D.: 1971, Astron. Astrophys. 14, 198.
Summers, H. P.: 1974, Internal Memo 367, Appleton Laboratory, Culham Laboratory, Abingdon, Oxon.
Walker, A. B. C., Jr., Rugge, H. R., and Weiss, K.: 1974a, Astrophys. J. 188, 423.
Walker, A. B. C., Jr., Rugge, H. R., and Weiss, K.: 1974b, Astrophys. J. 192, 169.
Walker, A. B. C., Jr., Rugge, H. R., and Weiss, K.: 1974c, Astrophys. J. 194, 471.
Wiese, W. L., Smith, M. W., and Glennon, M.: 1966, Atomic Transition Probabilities, Vol. 1, National Bureau of Standards, Washington.
Wiese, W. L., Smith, M. W., and Miles, B. M.: 1969, Atomic Transition Probabilities, Vol. 2, National Bureau of Standards, Washington.
Withbroe, G. L.: 1970, Solar Phys. 11, 42
Withbroe, G. L.: 1971a, Solar Phys. 18, 458.
Withbroe, G. L.: 1971b, Menzel Symposium on Solar Physics, Atomic Spectra, and Gaseous Nebulae, Special Report 353, National Bureau of Standards, Washington, p. 127.
Withbroe, G. L. and Gurman, J. B.: 1973, Astrophys. J. 183, 279.
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Withbroe, G.L. The analysis of XUV emission lines. Sol Phys 45, 301–317 (1975). https://doi.org/10.1007/BF00158452
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DOI: https://doi.org/10.1007/BF00158452