Space Science Reviews

, Volume 70, Issue 1–2, pp 379–386 | Cite as

Signature of coronal holes and streamers in the interplanetary space

  • Yuri I. Yermolaev
Coronal Holes and Solar Wind


The properties of different solar wind streams depend on the large scale structure of the coronal magnetic field. We present average values and distributions of bulk parameters (density, velocity, temperature, mass flux, momentum, and kinetic and thermal energy, ratio of thermal and magnetic pressure, as well as the helium abundance) as observed on board the Prognoz 7 satellite in different types of the solar wind streams. Maximum mass flux is recorded in the streams emanating from the coronal streamers while maximum thermal and kinetic energy fluxes are observed in the streams from the coronal holes. The momentum fluxes are equal in both types of streams. The maximum ratio of thermal and magnetic pressure is observed in heliospheric current sheet. The helium abundance in streams from coronal holes is higher than in streams from streamers, and its dependences on density and mass flux are different in different types of the streams. Also, the dynamics of α-particle velocity and temperature relative to protons in streams from coronal holes and streamers is discussed.

Key words

Sun Solar Wind Coronal Holes Streamers 


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  1. Geiss J.: 1985, inFuture Mission in Solar, Heliospheric and Space Plasma Physics, Garmisch-Partenkirshen, Germany, ESA SP-235, p. 37.Google Scholar
  2. Geiss, J., Hirt, P., Leutwyler, H.: 1970,Solar Phys. 12, 458.Google Scholar
  3. Hundhausen, A.J.: 1972, Coronal expansion and solar wind. Springer, Heidelberg, New York.Google Scholar
  4. Neugebauer, M.: 1981,Fund. Cosm. Phys. 7, 131Google Scholar
  5. Neugebauer, M.: 1982,Space Sci. Rev. 33, 127Google Scholar
  6. Parker, E.N.: 1963, Interplanetary Dynamical Processes. Interscience, New York.Google Scholar
  7. Schwenn, R.: 1986, inSpace Astronomy & Solar System Exploration, ESA SP-268, p. 131.Google Scholar
  8. Veselovsky, I.S.: 1984, inScience and Technology Results, Space Research 22, VINITI, Moscow, (in Russian).Google Scholar
  9. Withbroe, G.L.: 1986, inThe Sun and the Heliosphere in Three Dimensions, ed. R.G. Marsden, D. Reidel Publishing Company, p. 19.Google Scholar
  10. Yermolaev, Yu.I., Stupin, V.V.: 1990,Planet. Space Sci. 38, 1305.Google Scholar
  11. Yermolaev, Yu.I., Zastenker, G.N.: 1990,Kosmich. Issled. 28, 103 (in Russian).Google Scholar
  12. Yermolaev, Yu.I., 1991,Planet. Space Sci. 39, 1351Google Scholar
  13. Yermolaev, Yu.I.: 1992a, inStudy of the Solar-Terrestrial System, Proc. 26th ESLAB Symp., Killarney, 1992, ESA SP-346, p. 217.Google Scholar
  14. Yermolaev, Yu.I.: 1992b, inCorona Streamers, Coronal Loops, and Coronal and Solar Wind Composition, Proc. 1st SOHO Workshop, Annapolis, 1992, ESA SP-348, p. 339.Google Scholar

Copyright information

© Kluwer Academic Publishers 1994

Authors and Affiliations

  • Yuri I. Yermolaev
    • 1
  1. 1.Space Research InstituteRussian Academy of SciencesMoscowRussia

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