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Hydromagnetic Observations in the Solar Wind

  • K. W. Ogilvie
  • L. F. Burlaga
Part of the Astrophysics and Space Science Library book series (ASSL, volume 17)

Abstract

Experiments are conducted in the solar wind to determine the velocity distribution function of the plasma which is a function of time, space, and the species of particles studied. As has been pointed out (Vasyliunas, 1969) the length scale of the instruments used is so much less than any of the characteristic lengths of the plasma, that these instruments are just devices for the analysis and measurement of charged particle beams, and do not exploit directly any of the cooperative properties of the plasma. What is done is to determine the numbers of particles (dn)/(dv) dv in various differential regions of velocity space by counting them, and then either to fit to an assumed function, or use these values of differential density to approximate the unknown function. There are thus two problems which have been fully discussed by Vasyliunas:
  1. (a)

    The conversion of observed particle counts to values of (dn)/(dv) dv (the unfolding problem), which requires a good knowledge of the characteristics of the instrument; and

     
  2. (b)

    The approximation to the distribution function.

     

Keywords

Solar Wind Solar Phys Velocity Distribution Function Interplanetary Medium Solar Wind Parameter 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© D. Reidel Publishing Company, Dordrecht, Holland 1970

Authors and Affiliations

  • K. W. Ogilvie
    • 1
  • L. F. Burlaga
    • 1
  1. 1.Laboratory for Space SciencesNASA-Goddard Space Flight CenterGreenbeltUSA

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