Jove
Visualize
Contact Us
JoVE
x logofacebook logolinkedin logoyoutube logo
ABOUT JoVE
OverviewLeadershipBlogJoVE Help Center
AUTHORS
Publishing ProcessEditorial BoardScope & PoliciesPeer ReviewFAQSubmit
LIBRARIANS
TestimonialsSubscriptionsAccessResourcesLibrary Advisory BoardFAQ
RESEARCH
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchive
EDUCATION
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualFaculty Resource CenterFaculty Site
Terms & Conditions of Use
Privacy Policy
Policies

Related Experiment Videos

Coronal waves: propagation in the multi-fluid description.

Redouane Mecheri1, Eckart Marsch

  • 1Max Planck Institute for Solar System Research 37191 Katlenburg-Lindau, Germany. mecheri@mps.mpg.de

Philosophical Transactions. Series A, Mathematical, Physical, and Engineering Sciences
|January 18, 2006
PubMed
Summary
This summary is machine-generated.

Related Concept Videos

You might also read

Related Articles

Articles linked to this work by shared authors, journal, and citation graph.

Sort by
Same author

Proton core heating and beam formation via parametrically unstable Alfvén-cyclotron waves.

Physical review letters·2008
Same author

Solar wind origin in coronal funnels.

Science (New York, N.Y.)·2005
See all related articles

This study explores wave propagation in the solar corona using a multi-fluid model, revealing resonance frequencies important for coronal heating. These findings advance our understanding of plasma physics and solar atmosphere dynamics.

Area of Science:

  • Plasma Physics
  • Solar Physics
  • Astrophysics

Background:

  • Coronal plasma is a dynamic environment where wave phenomena are crucial.
  • Standard magnetohydrodynamics (MHD) models often neglect important kinetic effects like ion-cyclotron waves.
  • Understanding wave propagation is key to explaining energy transport and heating mechanisms in the solar corona.

Purpose of the Study:

  • To investigate wave propagation in low-beta coronal plasma.
  • To incorporate ion-cyclotron wave effects by using a collisionless multi-fluid model, going beyond traditional MHD.
  • To identify potential mechanisms for coronal heating through wave analysis.

Main Methods:

  • Utilized a collisionless multi-fluid model, neglecting electron inertia to include ion-cyclotron wave effects.

Related Experiment Videos

  • Performed a Fourier plane-wave perturbation analysis.
  • Numerically solved the derived dispersion relations for two- and three-fluid models.

    • Main Results:

    • Presented dispersion curves for the solar corona using representative plasma parameters.
    • Identified the presence of specific resonance frequencies within the analyzed plasma conditions.
    • Demonstrated that these resonance frequencies are a consequence of the multi-fluid approach and ion-cyclotron effects.

    Conclusions:

    • The identified resonance frequencies may play a significant role in the heating of the solar corona.
    • The multi-fluid model provides a more comprehensive description of wave phenomena in coronal plasma compared to MHD.
    • This research offers insights into energy transfer processes in astrophysical plasmas.