The spiral field inhibition of thermal conduction in two-fluid solar wind models

Details The spiral field inhibition of thermal conduction in two-fluid solar wind models The spiral field inhibition of thermal conduction in two-fluid solar wind models

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978jgr....83.3729n&link_type=abstract

Journal of Geophysical Research, vol. 83, Aug. 1, 1978, p. 3729-3739.

Physics

1

Conductive Heat Transfer, Interplanetary Magnetic Fields, Magnetic Field Configurations, Solar Wind, Thermal Conductivity, Two Fluid Models, Adiabatic Conditions, Density Distribution, Electron Energy, Lines Of Force, Mass Flow Rate, Proton Energy, Radial Flow, Solar Wind Velocity, Temperature Profiles, Three Dimensional Flow, Wave Equations

Scientific paper

The paper reports on two-field models which include the inhibition of thermal conduction by the spiraling interplanetary field to determine whether any of the major conclusions obtained by Nerney and Barnes (1977) needs to be modified. Comparisons with straight field line models reveal that for most base conditions, the primary effect of the inhibition of thermal conduction is the bottling-up of heat in the electrons as well as the quite different temperature profiles at a large heliocentric radius. The spiral field solutions show that coronal hole boundary conditions do not correspond to states of high-speed streams as observed at 1 AU. The two-fluid models suggest that the spiral field inhibition of thermal conduction in the equatorial plane will generate higher gas pressures in comparison with flows along the solar rotation axis (between 1 and 10 AU). In particular, massive outflows of stellar winds, such as outflow from T Tauri stars, cannot be driven by thermal conduction. The conclusions of Nerney and Barnes remain essentially unchanged.

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