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  • 1
    Electronic Resource
    Electronic Resource
    Ionospheric response to changes in the interplanetary magnetic field observed by EISCAT and AMPTE–UKS (1985)
    [s.l.] : Nature Publishing Group
    Nature 318 (1985), S. 451-452 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The AMPTE-UKS1 has a perigee of 550 km, apogee of 1.7 Earth radii and period of 43.8 h. In October 1984, apogee was near the noon meridian and the satellite was ideally situated to observe the IMF directly upstream of the Earth's magnetosphere and bow shock. The Imperial College magnetometer was ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/318451a0
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    Use of Al xii and Mg xi lines as solar plasma diagnostics (1989)
    Springer
    Solar physics 124 (1989), S. 289-302 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present three sets of observations of n = 1 to n = 2 lines due to helium-like aluminium (Alxii), made during two solar flares (25 August, 1980 and 19 October, 1986), using the X-Ray Polychromator on the SMM satellite. The observed temperature-sensitive line ratio G is shown to be consistent with the close-coupling calculations of Keenan and McCann (1987), although the ratio R, which is both temperature and density-sensitive for lower-Z elements, is not sufficiently well determined from these data to say more than that the observed values of R are not inconsistent with the theoretical calculations. This region of the spectrum also includes the helium-like magnesium (Mgxi) 11 S - 31 P line, and it is shown that the ratio of this line to the Alxii resonance (11 S - 21 P) line is a more sensitive indicator of electron temperature than are the Alxii G and R ratios. We demonstrate that the three ratios may be used together in order to derive values of emission measure, electron temperature and electron density during these flares.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00156271
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    Paper (German National Licenses)
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  • 3
    Electronic Resource
    Electronic Resource
    Application of Spectroscopic Diagnostics to Early Observations with the SOHO Coronal Diagnostic Spectrometer (1997)
    Springer
    Solar physics 170 (1997), S. 143-161 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Coronal Diagnostic Spectrometer (CDS) has as a scientific goal the determination of the physical parameters of the solar plasma using spectroscopic diagnostic techniques. Absolute intensities and intensity ratios of the EUV spectral emission lines can be used to obtain information on the electron density and temperature structure, element abundances, and dynamic nature of different features in the solar atmosphere. To ensure that these techniques are accurate it is necessary to interface solar analysis programs with the best available atomic data calculations. Progress is reported on this work in relation to CDS observations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1004997003844
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    Paper (German National Licenses)
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  • 4
    Electronic Resource
    Electronic Resource
    EUV Observations Above Polar Coronal Holes (1999)
    Springer
    Space science reviews 87 (1999), S. 185-188 
    Details
    ISSN: 1572-9672
    Keywords: solar corona ; coronal holes ; electron temperature ; electron density
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We derive electron temperature and density as a function of height up to 0.2 R⊙ above the limb in polar coronal holes, using five EUV data sets recorded by the SOHO Coronal Diagnostic Spectrometer between July 1997 and February 1998. Radial T and N distributions, averaged in a 2° to 10° range of position angles, are the same above the North and South coronal holes. They do not show any time variability over a period of seven months. Polar plumes are found to have lower electron temperature and higher density than the interplume lanes. The electron density slope suggests that the proton temperatures are twice as high as the electron temperatures.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005127930584
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  • 5
    Electronic Resource
    Electronic Resource
    The Solar Magnetic Field as a Coronal Hole Extension Forms: Effects of Magnetic Helicity and Boundary Conditions (1999)
    Springer
    Space science reviews 87 (1999), S. 145-148 
    Details
    ISSN: 1572-9672
    Keywords: force-free ; corona ; magnetic fields
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract An analytical solution is presented for linear force fields within a spherical shell, representing the solar corona. Allowing for a global magnetic helicity, we find magnetic fields over the entire corona with realistic inner boundary conditions obtained from transformation and extrapolation of photospheric magnetograms and considering alternative outer boundary conditions. Such fields are found for the well known coronal hole extension event of August 1996.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005190821498
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  • 6
    Electronic Resource
    Electronic Resource
    Characterization of Solar Coronal Holes and Plumes Using Spectroscopic Diagnostic Techniques Applied to SOHO/CDS Observations (1999)
    Springer
    Space science reviews 87 (1999), S. 169-172 
    Details
    ISSN: 1572-9672
    Keywords: solar corona ; spectroscopic diagnostics ; plumes
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Results from a series of SOHO/Coronal Diagnostic Spectrometer (CDS) observations of coronal holes and plumes are presented, including analysis of a low-latitude plume observed in August 1996. Spectroscopic diagnostic techniques using the CHIANTI atomic database are applied to derive the plasma parameters: electron density, temperature, and element abundances. The results are compared with quiet sun values. Coronal electron densities in the holes are found to be about 2 × 108 cm-3, a factor of two to three lower than in the quiet sun. The plasma thermal distribution exhibits differences between coronal holes, the quiet sun and plumes. For example, the peak of the emission in coronal holes is at a lower temperature (T ⋍ 8 × 105 K) than in the quiet sun (T ⋍ 1 × 106 K), while plumes are cooler (T ⋍ 7.6 × 105 K) and show a different distribution, closer to an isothermal state.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005111426041
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    Paper (German National Licenses)
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