Wave speeds in the corona and the dynamics of mass ejections

Details Wave speeds in the corona and the dynamics of mass ejections Wave speeds in the corona and the dynamics of mass ejections

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sfcp.rept..262s&link_type=abstract

In its Solar Flares and Coronal Physics Using P/OF as a Research Tool p 262-267 (SEE N86-24614 14-92)

Physics

Advection, Dynamic Characteristics, Mass Flow, Solar Corona, Solar Wind, Wave Fronts, Density (Mass/Volume), Magnetic Fields, Magnetohydrodynamics, Models, Temperature

Scientific paper

A disturbance or coronal mass ejection being advected by the solar wind will expand at the fastest local characteristic speed - typically approximately the fast-mode speed. To estimate this characteristic wave speed and the velocity field in the ambient corona, it is necessary to know the magnetic field, temperature, and density. Only the density is known from coronal observations. The temperature, magnetic field, and velocity are not yet directly measured in the outer corona and must be estimated from a model. In this study, it is estimated that the magnetic field, solar wind velocity, and characteristic speeds use the MHD model of coronal expansion between 1 and 5 solar radii (R solar radii) with a dipole magnetic field at the base. This model, for a field strength of about 2 gauss at the base, gives flow speeds at low latitudes (near the heliospheric current sheet) of 250 km/s at 5 R solar radii and, 50 km/s at 2 solar radii, and fast-mode speeds to 400 to 500 km/s everywhere between 2 and 5 solar radii. This suggests that the outer edge of a velocity of mass ejection reported by MacQueen and Fisher (1983) and implies that the acceleration mechanism for coronal mass ejections is other than simple entrainment in the solar wind.

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