The power spectrum of Alfvenic fluctuations propagating in nonisotropic solar wind

Details The power spectrum of Alfvenic fluctuations propagating in nonisotropic solar wind The power spectrum of Alfvenic fluctuations propagating in nonisotropic solar wind

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989cha%26a..13..105t&link_type=abstract

Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 13, March 1989, p. 105-117. Translation.

Astronomy and Astrophysics

Astrophysics

Magnetohydrodynamic Waves, Power Spectra, Solar Wind, Wave Propagation, Anisotropy, Magnetic Field Configurations, Solar Protons

Scientific paper

The power spectrum equation of Tu et al. (1986) for Alvenic fluctuations propagating in an isotropic plasma is extended for the case of propagation through an anisotropic medium. It is assumed that the Alfvenic fluctuation is in an asymmetrical MHD turbulent state between 0.3 and 1 AU. The equations neglect the radial variation of each component, the gradient of the velocity perturbation vector in the moment equation, and small scale variations in the density.

Affiliated with

Also associated with

No associations

Rating

The power spectrum of Alfvenic fluctuations propagating in nonisotropic solar wind does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The power spectrum of Alfvenic fluctuations propagating in nonisotropic solar wind, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The power spectrum of Alfvenic fluctuations propagating in nonisotropic solar wind will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1803134