Solar flare X-ray spectra from the Solar Maximum Mission Flat Crystal Spectrometer

1982 ◽  
Vol 256 ◽  
pp. 774 ◽  
Author(s):  
K. J. H. Phillips ◽  
B. C. Fawcett ◽  
B. J. Kent ◽  
A. H. Gabriel ◽  
J. W. Leibacher ◽  
...  
Keyword(s):  
Solar Flare ◽  
Solar Maximum ◽  
Crystal Spectrometer ◽  
Solar Maximum Mission ◽  
X Ray

Atomic physics calculations relevant to solar flare spectra

1991 ◽  
Vol 336 (1643) ◽  
pp. 471-484 ◽  
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 .

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

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.

The role of magnetic loops in solar flares

1991 ◽  
Vol 336 (1643) ◽  
pp. 389-400 ◽  
Keyword(s):  
Solar Flare ◽  
Spatial Structure ◽  
Spatial Resolution ◽  
Solar Flares ◽  
Solar Maximum ◽  
Magnetic Topology ◽  
Solar Maximum Mission ◽  
X Ray ◽  
Ultraviolet Observations

X -ray and ultraviolet observations of flares have provided much important information on their spatial structure and magnetic topology. The early observations from Skylab emphasized the role of simple loops and loop arcades, but later observations from the Solar Maximum Mission have greatly complicated this picture. Flares appear in a multitude of loops with complex spatial and temporal interrelations. In many cases, interactions between different loops appear to play a crucial role. The inferred magnetic topology of solar flares will be reviewed with emphasis on the implications for processes of energy release and transfer. It will be shown that the spatial resolution of the observations obtained so far is still inadequate for solving many basic questions of solar flare research.

scholarly journals Plasma Parameters and Structures of the X4 Flare of 19 May 1984 as Observed by SMM-XRP

1989 ◽  
Vol 104 (2) ◽  
pp. 165-168
Author(s):  
J.T. Schmelz ◽  
J.L.R. Saba ◽  
K.T. Strong
Keyword(s):  
Solar Maximum ◽  
Coronal Plasma ◽  
The Sun ◽  
Plasma Parameters ◽  
Crystal Spectrometer ◽  
Solar Maximum Mission ◽  
X Ray ◽  
Bent Crystal ◽  
East Limb ◽  
Large Flare

AbstractThe eruption of a large flare on the east limb of the Sun was observed by the X-Ray Polychromator (XRP) on board the Solar Maximum Mission (SMM) on 19 May 1984. The XRP Flat Crystal Spectrometer (FCS) made polychromatic soft X-ray images during the preflare, flare and postflare phases. The XRP Bent Crystal Spectrometer (BCS) provided information on the temperature and dynamics of the hot (Te > 8 x 106K) coronal plasma from spectra integrated spatially over the whole region.

scholarly journals Preface

1991 ◽  
Vol 336 (1643) ◽  
pp. 323-323
Keyword(s):  
Solar Flare ◽  
Energy Release ◽  
Gamma Rays ◽  
Solar Flares ◽  
Solar Maximum ◽  
Interplanetary Space ◽  
Release Site ◽  
Solar Maximum Mission ◽  
New Information ◽  
Three Space

During the period of the 1980 solar maximum three space missions (P78-1, Solar Maximum Mission and Hinotori ) carried out extensive studies of solar flares. In their different ways all of these missions contributed significant new information to our understanding of the solar flare phenomenon. In this volume the contribution made by these three spacecraft to the study of the energy release and the related creation of high-tem perature plasma, the transport of energy from the primary release site, the production of gamma-rays at energies up to 10 MeV and the ejection of solar matter into interplanetary space are reviewed.

Solar flare plasmas

1981 ◽  
Vol 300 (1456) ◽  
pp. 497-504
Keyword(s):  
Energy Storage ◽  
Solar Flare ◽  
Energy Release ◽  
Solar Maximum ◽  
Theoretical Modelling ◽  
Solar Maximum Mission ◽  
Mission Satellite ◽  
Storage Energy ◽  
Three Phases

The solar flare is discussed in terms of its three phases: energy storage, energy release, and dissipation. Some of the problems associated with theoretical modelling are considered, together with the limitations imposed by current observations. New measurements to be made by the N.A.S.A. Solar Maximum Mission satellite are expected to advance significantly our understanding of the flare mechanism.

scholarly journals Distorted Wave Calculations: Application to Astrophysics and Tokamak Plasma

1984 ◽  
Vol 86 ◽  
pp. 92-99
Author(s):  
A.K. Bhatia
Keyword(s):  
Physical Properties ◽  
Spectral Resolution ◽  
Spectroscopic Data ◽  
Solar Maximum ◽  
Tokamak Plasma ◽  
Line Profiles ◽  
Distorted Wave ◽  
Solar Maximum Mission ◽  
X Ray ◽  
Line Intensities

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.

Sign in / Sign up

Export Citation Format

Share Document