Interpretation of the X-Ray Spectra of Solar Active Regions

Walker, Arthur B. C.

doi:10.1007/978-94-010-1802-9_10

Cited by 7 publications

(1 citation statement)

References 61 publications

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“…The "kernel" of the integral, K(T.,), which is the convolution of the telescope efficiency and the solar emissivity, is given by a ? sum indexed by element (Z), ionization stage (z), and transition from excited state i to lower state j K(T) = : ic1( X) = : (5) k Zzij where A is the abundance of element Z, a is the fractional population of ionization stage z, and aZZ is the excitation function for transition (i->j) (including all population processes for the upper level i, and branching ratios to the lower level j). These relations only hold for optically thin lines; thus, this derivation is not valid for the 1216 A telescope, which is sensitive to the optically thick Lyman a line6.…”

Section: Solar Emissionmentioning

confidence: 99%

Performance of the Multi-Spectral Solar Telescope Array V: temperature diagnostic response to the optically thin solar plasma

DeForest

Kankelborg

Allen

et al. 1991

X-Ray/Euv Optics for Astronomy, Microscopy, Polarimetry, and Projection Lithography

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We have developed compact soft x-ray, extreme ultraviolet (BUY), and far-ultraviolet (FUV) multilayer coated telescopes for the study of the solar chromosphere, corona, and corona/solar wind interface. Because these systems operate at short wavelengths (-40 A <2 < 1550 A), the modest apertures of4O mm -127 mm allow observations at very high angular resolution (0. 1 -0.7 arc second). In addition to permitting traditional normal incidence optical configurations (such as Cassegrain, Ritchey-Chrétien, and Herschelian configurations) to be used at soft x-ray/EUV wavelengths, multilayer coatings also allow a narrow wavelength band (/& -15 -100) to be selected for imaging. The resulting telescopes provide a very powerful and flexible diagnostic instrument for the study of both the fine scale structure of the chromosphere/corona interface and the large scale structure of the corona and corona/solar wind interface. In previous papers we have described a new solar rocket payload, the Multi-Spectral Solar Telescope Array (MSSTA), which is composed of 17 of these compact telescopes. In the present paper, we report on the ability of the MSSTA payload to obtain temperature diagnostic information about the optically thin solar plasma. We also discuss applications of this information to studies of coronal structure.

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Section: Solar Emissionmentioning

confidence: 99%

Performance of the Multi-Spectral Solar Telescope Array V: temperature diagnostic response to the optically thin solar plasma

DeForest

Kankelborg

Allen

et al. 1991

X-Ray/Euv Optics for Astronomy, Microscopy, Polarimetry, and Projection Lithography

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X-Ray Spectra of Solar Active Regions

Parkinson

1975

Solar Gamma-, X-, and EUV Radiation

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Multitemperature analysis of solar X-ray line emission

1980

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In this paper we propose and test a new method of multitemperature analysis of solar X-ray spectra. The method, which is based on a technique developed by Withbroe (1975), is designed to be used in the interpretation of spectra, to be measured by the X-Ray Polychromator on the Solar Maximum Mission. Various tests of the method on simulated temperature models establish its usefulness, generality, and stability. The possibilities of deriving the relative element abundances are analysed. The results of the present paper extend the possibility of the multitemperature analysis of X-ray spectra as compared with the results of Craig and Brown (1976a, b) and Craig (1977).

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Interpretation of the X-Ray Spectra of Solar Active Regions

Cited by 7 publications

References 61 publications

Performance of the Multi-Spectral Solar Telescope Array V: temperature diagnostic response to the optically thin solar plasma

Performance of the Multi-Spectral Solar Telescope Array V: temperature diagnostic response to the optically thin solar plasma

X-Ray Spectra of Solar Active Regions

Multitemperature analysis of solar X-ray line emission

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