Physics
Scientific paper
Dec 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442...41a&link_type=abstract
In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 41-45 (SEE N87-20871 13-92)
Physics
3
Cylindrical Plasmas, Magnetic Field Configurations, Magnetohydrodynamic Stability, Solar Corona, Solar Magnetic Field, Solar Physics, Solar Prominences, Sun, Heat Transfer, Plasma Temperature
Scientific paper
Condensation modes in magnetized cylindrical plasmas, with concentration on how magnetic field affects the stability were studied. It is found that the effects of magnetic field (shear, twist, and strength) on the condensation modes are different depending on the wave vector. For modes whose wave vector is not perpendicular to magnetic field lines the plasma motion is mainly along the field lines; the effects of magnetic field on the modes are negligible except on the heat flow parallel to the field line. For a mode which is localized near a surface where the wave vector is perpendicular to the field line, the plasma moves perpendicular to the line carrying the field line into the condensed region; magnetic field affects the mode by building up magnetic pressure in the condensed region. The stability of condensation modes strongly depends on how density and temperature vary with field twist. The stable nature of global quiescent prominence magnetic configurations implies that prominences form for low field twist for which ideal MHD modes are stable; plasma temperature should increase with field twist for stable prominence formation.
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