The sheath/ionosphere boundary layer at Venus

K. Szegö, V. D. Shapiro, S. K. Ride, A. F. Nagy, V. I. Shevchenko

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3 Citations (Scopus)


At Venus the interaction of the shocked solar wind and cold planetary ions takes place in the dayside mantle. The shocked solar wind is a warm, drifting Maxwellian plasma whereas the planetary plasma is cold; the plasma in the mantle is strongly magnetized. The coexistence of these two populations is unstable, and it leads to wave excitations that organize the energy and momentum exchange between the shocked solar wind and the plasma of planetary origin. The source of the free energy is the solar wind. The intensive wave activity seen in the 100 Hz channel of the wave instrument onboard the Pioneer-Venus Orbiter in the dayside mantle region of Venus can be identified as almost electrostatic VLF waves excited by the kinetic branch of the modified two-stream lower hybrid instability. The waves interact with the particles, and the planetary plasma is heated and accelerated outside the ionosphere, close to its upper boundary. This way solar wind scavenges the ionosphere, and planetary ions leave the planetary magnetosphere. A portion of the wave energy is capable to penetrate directly into the ionosphere and heats it.

Original languageEnglish
Pages (from-to)71-74
Number of pages4
JournalAdvances in Space Research
Issue number4
Publication statusPublished - 1995

ASJC Scopus subject areas

  • Aerospace Engineering
  • Astronomy and Astrophysics
  • Geophysics
  • Atmospheric Science
  • Space and Planetary Science
  • Earth and Planetary Sciences(all)

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    Szegö, K., Shapiro, V. D., Ride, S. K., Nagy, A. F., & Shevchenko, V. I. (1995). The sheath/ionosphere boundary layer at Venus. Advances in Space Research, 16(4), 71-74.