MHD modes of solar wind flow tubes.

Details MHD modes of solar wind flow tubes. MHD modes of solar wind flow tubes.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...311..311n&link_type=abstract

Astronomy and Astrophysics, v.311, p.311-316

Astronomy and Astrophysics

Astrophysics

23

Mhd, Waves, Solar Wind, Sun: Magnetic Fields

Scientific paper

The properties of linear magnetosonic waves trapped within solar wind flow tubes are considered. The trapping is due to reflection of the waves from the tube boundary, which may correspond to either a jump in plasma density or magnetic field, or a jump in the steady flow velocity. The structure of the waves transverse to the magnetic field is defined by the boundary conditions. The phase and group speeds of the waves depend upon the wave frequency and wavelength. For realistic conditions in a flow tube, corresponding to a "spaghetti structure", there are two types of trapped waves propagating away from the Sun, fast and slow waves. These waves are "backward", in the sense that they would propagate towards the Sun in the absence of any difference in the steady flow velocity inside and outside the tube. The "forward" magnetosonic waves are not trapped under solar wind conditions. Both slow and fast backward waves have phase velocities that are sub-Alfvenic. There are no MHD waves propagating towards the Sun.

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