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Träfflista för sökning "WFRF:(Wahlgren G. M) srt2:(1995-1999)"

Search: WFRF:(Wahlgren G. M) > (1995-1999)

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1.
  • Larsson, Gerry, et al. (author)
  • The Grossarth-Maticek and Eysenck personality types, health-related behaviour, and indicators of transitory ill-health
  • 1995
  • In: European Journal of Personality. - : SAGE Publications. - 0890-2070 .- 1099-0984. ; 9:2, s. 75-87
  • Journal article (peer-reviewed)abstract
    • The aim of this study was to scrutinize the relationship between personality type as described by Grossarth-Maticek and Eysenck, health-related behaviours, and indicators of transitory ill health in a community sample. The sample consisted of all per sons aged 40 years (45 men and 35 women) in a Swedish municipality who agreed to take part in a health examination at the primary health care centre of the municipality. The Short Interpersonal Reactions Inventory (Grossarth-Maticek and Eysenck, 1990) was used to measure personality type. Self-report data were obtained regarding seven health-related behaviours. Health was assessed in three ways; self-report (paper and pencil), self-report (interview response to physician), and measures of 36 biological variables including immune system indicators. The allocation of persons to the different personality types proved problematic using the established methods. By combining the types, according to Eysenck's personality model, and performing a cluster analysis on this combination, a ‘healthy’ and a ‘stressed’ profile were identified within both the male and the female group of subjects. Persons in the healthy personality cluster showed more favourable scores on the health-related behaviour indices and on the self-report health scales than the persons in the stressed cluster. They also tended to score lower than those in the stressed cluster on most of the biological markers known to increase during acute stress. The possibility that this implies a higher level of strain for the persons in the stressed cluster on various bodily systems is discussed.
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2.
  • Lundberg, Hans, et al. (author)
  • Experimental Pd II oscillator strengths and the palladium abundance in the HgMn-type star chi Lupi
  • 1996
  • In: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 469:1, s. 388-392
  • Journal article (peer-reviewed)abstract
    • Experimental oscillator strengths for 19 ultraviolet lines of Pd II have been derived from measurements of line intensities in calibrated Fourier transform spectra, combined with picosecond-pulse laser measurements of radiative lifetimes. Five of these 19 lines, in addition to other Pd nr lines, are present in Hubble Space Telescope/Goddard High-Resolution Spectrograph echelle spectra of the chemically peculiar HgMn star chi Lupi, yielding a palladium abundance of log (N-Pd) = +5.0, which is 3.3 dex above the solar abundance. Theoretical oscillator strengths have been calculated for all strong ultraviolet transitions associated with the lowest odd-parity configuration of Pd II.
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3.
  • Sikstrom, C. M, et al. (author)
  • New Zr II oscillator strengths and the zirconium conflict in the HgMn star chi Lupi
  • 1999
  • In: Astronomy & Astrophysics. - 0004-6361. ; 343:1, s. 297-302
  • Journal article (peer-reviewed)abstract
    • Lifetimes on the sub-nanosecond scale for the levels v(2)D(3/2), v(2)F(3/2) and v(2)F(5/2) in the 4d5s5p configuration in Zr II have been measured, using the method of laser-induced fluorescence. Combined with branching fractions obtained with the Lund Ultraviolet (UV) Fourier Transform Spectrometer (FTS), experimental oscillator strengths have been derived. From Hubble Space Telescope/Goddard High-Resolution Spectrograph spectra, the zirconium abundance in the HgMn star chi Lupi has been determined from Zr II and Zr III lines. More than an order of magnitude difference in the Zr II abundance has been derived from these ionization stages. The difference is much too large to be explained by uncertainties in the oscillator strengths. Possible explanations of this difference have to be found in the stellar models, such as the influence of non-LTE or diffusion.
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  • Result 1-4 of 4

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