Distorted Wave Calculations: Application to Astrophysics and Tokamak Plasma

During the last few years, observations of solar phenomena have been carried out by rocket flights, manned satellites like Skylab, unmanned satellites like Orbiting Solar Observatories and more recently Solar Maximum Mission. The wavelengths, line intensities and line profiles in UV and X-ray regions of the solar spectra have been measured. The spectroscopic data obtained are of high spatial and spectral resolution. The goal is to understand the physical properties of the emitting plasma and determine the electron temperatures, densities and volume of the emitting plasma from UV and X-ray spectra.

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Soft X-Ray Spectroscopy from the X-Ray Polychromator on the Newly Repaired Solar Maximum Mission

International Astronomical Union Colloquium ◽

10.1017/s0252921100085158 ◽

1984 ◽

Vol 86 ◽

pp. 9-11

Author(s):

K.T. Strong ◽

R.A. Stern ◽

J.R. Lemen ◽

K.J.H. Phillips

Keyword(s):

Spectroscopic Data ◽

Solar Maximum ◽

Active Regions ◽

Line Profiles ◽

Crystal Spectrometer ◽

Solar Maximum Mission ◽

X Ray ◽

Bent Crystal ◽

Mission Satellite ◽

Short Presentation

The X-Ray Polychromator (XRP) resumed operations on 24 April 1984 following the successful in-orbit repair of the Solar Maximum Mission Satellite. Since that time the two instruments that comprise the XRP, the Flat Crystal Spectrometer (FCS) and the Bent Crystal Spectrometer (BCS), have been used to obtain new spectroscopic data from active regions and flares. The FCS, in particular, has accumulated far more observations of soft X-ray line profiles than were obtained during SMM-I in 1980. For this short presentation, we have chosen two topics to illustrate the type of data that we have obtained since the repair.

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Properties of an impulsive compact solar flare determined from Solar Maximum Mission X-ray measurements

The Astrophysical Journal ◽

10.1086/166620 ◽

1988 ◽

Vol 331 ◽

pp. 1036 ◽

Cited By ~ 22

Author(s):

G. A. Linford ◽

C. J. Wolfson

Keyword(s):

Solar Flare ◽

Solar Maximum ◽

Solar Maximum Mission ◽

X Ray

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Flat Crystal X-Ray Optics

Advances in X-ray Analysis ◽

10.1154/s0376030800000161 ◽

1957 ◽

Vol 1 ◽

pp. 193-206 ◽

Cited By ~ 1

Author(s):

William J. Campbell ◽

Melvin Leon ◽

John Thatcher

Keyword(s):

Wave Length ◽

Pulse Height ◽

Line Profiles ◽

Line Broadening ◽

Crystal Surfaces ◽

X Ray ◽

Line Intensities ◽

Long Wave ◽

On Line ◽

College Park

AbstractAn investigation was undertaken by the Bureau of Mines at College Park, Md., to determine the effect of various combinations of collimators, analyzing crystals and detectors on line intensities, line-to-backgrouhd ratios, and spectral resolution. The research showed that line broadening due to mosaic crystal surfaces was greatly reduced and line splitting from faults was eliminatedby the use of two fine collimators (0.005 inch, spacing, 4 inch length). Line intensities were reduced, but lineto- background ratios arid line profiles were substantially improved with double collimators. Pulse height discrimination resulted in marked improvement in the line-to-background ratio in the long-wave length region, 2 to 10 A, but was much less effective for shorter wave lengths.

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Atomic physics calculations relevant to solar flare spectra

Philosophical Transactions of the Royal Society of London Series A Physical and Engineering Sciences ◽

10.1098/rsta.1991.0096 ◽

1991 ◽

Vol 336 (1643) ◽

pp. 471-484 ◽

Cited By ~ 2

Keyword(s):

Solar Flare ◽

Atomic Physics ◽

Solar Flares ◽

Solar Maximum ◽

Emission Lines ◽

Atomic Data ◽

Solar Maximum Mission ◽

X Ray ◽

Physical Conditions ◽

Recombination Processes

Solar flare spectra in the ultraviolet and X-ray wavelength regions are rich in emission lines from highly ionized ions, formed at temperatures around 10 7 K. These lines can be used as valuable diagnostics for probing the physical conditions in solar flares. Such analyses require accurate atomic data for excitation, ionization and recombination processes. In this paper, we present a review of work which has already been carried out, in particular for the Solar Maximum Mission observations, and we look to future requirements for Solar-A .

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