Journal of The Korean Astronomical Society (천문학회지)

The Korean Astronomical Society (한국천문학회)
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NUMERICAL CALCULATION OF TWO FLUID SOLAR WIND MODEL

  • KIM S.-J. (Korea Astronomy Observatory, Department of Astronomy & Space Science, Kyunghee University) ;
  • KIM K.-S. (Department of Astronomy & Space Science, Kyunghee University) ;
  • MOON Y.-J. (Korea Astronomy Observatory) ;
  • CRO K.-S. (Korea Astronomy Observatory) ;
  • PARK Y. D. (Korea Astronomy Observatory, Big Bear Solar Observatory, NJIT)
  • Published : 2004.03.01
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Abstract

We have developed a two fluid solar wind model from the Sun to 1 AU. Its basic equations are mass, momentum and energy conservations. In these equations, we include a wave mechanism of heating the corona and accelerating the wind. The two fluid model takes into account the power spectrum of Alfvenic wave fluctuation. Model computations have been made to fit observational constraints such as electron($T_e$) and proton($T_p$) temperatures and solar wind speed(V) at 1 AU. As a result, we obtained physical quantities of solar wind as follows: $T_e$ is $7.4{\times}10^5$ K and density(n) is $1.7 {\times}10^7\;cm^{-3}$ in the corona. At 1 AU $T_e$ is $2.1 {\times} 10^5$ K and n is $0.3 cm^{-3}$, and V is $511 km\;s^{-1}$. Our model well explains the heating of protons in the corona and the acceleration of the solar wind.

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  3. A Review on Solar Wind Modeling: Kinetic and Fluid Aspects vol.32, pp.1, 2011, https://doi.org/10.1007/s10712-010-9106-y