![]() ![]() ![]() Wilson, R.: 1964, ‘The Zeta/Solar lines Between 170 Å and 220 Å IAU Symp. Wilson, O.C.: 1963, ‘A Probable Correlation Between Chromospheric Activity and Age in Main-Sequence Stars’, Astrophys. Vaughan, A.H.: 1980, ‘Comparison of Activity Cycles in Old and Young Main-Sequence Stars’, Publ. and Rosner, R.: (1978), ‘Recent Advances in Coronal Physics’, Ann. Vaiana, G.S., et al.: 1981, ‘Results from an Extensive EINSTEIN Stellar Survey’, Astrophys. In solar and heliophysics the coronal heating problem relates to the puzzle of identifying and understanding the mechanism(s) causing the coronas temperatures. and Timothy, A.F.: 1973, ‘Identification and Analysis of Structures in the Corona’, Sol. 1988, The Physics of Solar Flares, Cambridge University Press, UK. Hudson, Universal Academy Press, Tokyo, Japan. Shimizu, T.: 1994, ‘Active Region Transient Brightenings’, in X-ray Solar Physics from Yohkoh, eds. Shimizu, T., Tsuneta, S., Acton, L.W., Lemen, J.R., and Uchida, Y.: 1992, ‘Transient Brightenings in Soft X-rays Observed by the Soft X-ray Telescope on Yohkoh’, Publ. and Golub, L.: 1979, ‘Rapid Changes in the Fine Structure of a Coronal Bright Point and a Small Coronal Active Region’, Sol. and Harvey, J.W.: 1980, ‘Observations of Magnetic Fields on Two Late-Type Dwarf Stars’, Astrophys. (eded.) 1981, Solar Active Regions, Colorado Assoc. and Ulmschneider, P.: 1990, ‘Chromospheric and Coronal Heating Mechanisms’, Space Sci. and Haisch, B.M.: 1979, ‘Outer Atmospheres of Cool Stars I″’, Astrophys. Linsky, J.L.: 1980, ‘Stellar Chromospheres’, Ann. and Wilson, R.: 1968, ‘XUV and Soft X-ray Spectra of the Sun’, Nature 219, 252. Harvey-Angle, K.L.: 1993, ‘Magnetic Bipoles on the Sun’, Ph.D. and Vaiana, G.S.: 1974, ‘Solar X-ray Bright Points’, Astrophys. Golub, L., Krieger, A.S., Silk, J.K., Timothy, A.F. and Wilczynski, J.: 1990, ‘Sub-arcsecond Observations of the Solar X-ray Corona’, Nature, No. Golub, L., Herant, M., Kalata, K., Lovas, S., Nystrom, G., Pardo, F., Spiller, E. Golub, L.: 1980, ‘Solar X-ray Bright Points’, Phi. Golub, L.: 1991, ‘X-ray Observations of Global Solar Activity’, in Flare Physics in Solar Activity Maximum 22, ed. and Stenflo, J.O.: 1972, ‘On the Small-Scale Structure of Solar Magnetic Fields’, Sol. 70, 781.ĭunn, R.B.: 1971, Coronal Events Observed in 5303Å in Physics of the Solar Corona, ed. and Tousey, R.: 1946, ‘Solar Ultraviolet Spectrum to 88 km’, Phys. The density structure of polar plumes, which are thought to contribute to the solar wind, has been derived from the observations out to 1.7 solar radii.Baum, W.A., Johnson, F.S., Oberly, J.J., Rockwood, C.C., Strain, C.V. Many features of coronal structure, including magnetically confined loops of hot plasma, coronal plumes, polar coronal holes, faint structures on the size scale of supergranulation and smaller, and features due to overlying cool prominences are visible in the images. The images have angular resolution of about 1.0 to 1.5 arc seconds, and show no degradation because of x-ray scattering. This emission is from coronal plasma in the temperature range 0.8 x 10(6) to 1.4 x 10(6)K. The bandpass centered at 173 angstroms is dominated by emission from the ions Fe IX Fe X. However, when the sun is totally the corona is in fact so high that it emits copious eclipsed, a white halo appears around the edge of the amounts of X-ray. The Cassegrain telescopes provided images in bands centered at 173 and 256 angstroms. The inherent energy-selective property of multilayer-coated optics allowed distinct groups of emission lines to be isolated in the solar corona and the transition region. High-resolution images of the sun in the soft x-ray to extreme ultraviolet(EUV) regime have been obtained with normal-incidence Cassegrain multilayer telescopes operated from a sounding rocket in space. ![]()
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