The solar wind mass flux

Details The solar wind mass flux The solar wind mass flux

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...337l..49w&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 337, Feb. 1, 1989, p. L49-L52.

Astronomy and Astrophysics

Astrophysics

24

Solar Corona, Solar Flux, Solar Wind, Electron Density (Concentration), Energy Dissipation, Energy Transfer, Gas Pressure, Particle Flux Density, Solar Radiation

Scientific paper

One of the unexplained observations of the solar wind at 1 AU is the relative constancy of the solar wind mass flux. Calculations using a radiative energy balance model with a thermally driven wind suggest that this near constancy of the mass (particle) flux is due to two factors: (1) the role of inward conduction and radiation in cooling the corona, and (2) the finding that the particle flux is proportional to the gas pressure in the outer corona and beyond, where the solar wind flow becomes radial.

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