Solar Physics

, Volume 165, Issue 1, pp 115–137

Two dynamical models for solar spicules

  • Paul Lorrain
  • Serge Koutchmy
Article

DOI: 10.1007/BF00149093

Cite this article as:
Lorrain, P. & Koutchmy, S. Sol Phys (1996) 165: 115. doi:10.1007/BF00149093

Abstract

Solar spicules are luminous jets that erupt up to 10 000 km from the surface of the Sun and have diameters, all along their length, of only about 150–200 km. We first review some recent observations made at the Hα wavelength. According to our models, a solar spicule is a self-channelled proton beam emitted by a magnetic element and surrounded by a cold sheath. The beam originates in a self-excited dynamo that exploits a v × B field and that could be situated either below or above the element, where v is the local plasma velocity and B is the local magnetic flux density. In falling back, the sheath provides a return current of protons that cancels the outgoing current. We discuss the channelling of charged-particle beams of very large cross-section and propose velocity channelling, which is apparently a new concept. We assume a steady state and a hydrogen plasma.

Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • Paul Lorrain
    • 1
    • 2
  • Serge Koutchmy
    • 3
  1. 1.Department of Earth and Planetary SciencesMcGill University, 3450 rue UniversitéMontréalCanada
  2. 2.Institut d'Astrophysique de Paris, CNRSParisFrance
  3. 3.Institut d'Astrophysique de Paris, CNRSParisFrance