CONDUCTIVE HEATING OF THE SOLAR WIND. PART I
CONDUCTIVE HEATING OF THE SOLAR WIND. PART I
复制标题
太阳风传导加热。
DOI：
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发表时间：
1963
期刊：
影响因子：
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通讯作者：
F. Scarf
中科院分区：
文献类型：
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作者：
L. M. Noble;F. Scarf
本文求解了在薄壳外无外热源的日冕快速膨胀情况下的流体动力学方程。假设日冕中约有10%的氦离子，而查普曼的无阻热导率值在任何地方都可以使用。在IBM 7090计算机上对方程进行积分，从地球到太阳，在r/sub c/处的奇点附近采用幂级数展开，其中kT（r/sub c/）= mu/sup 2/（r/sub c/）。结果发现，如果内日冕密度接近可接受的值，基础温度接近2 × 10 ~ 6/sup/ deg K，热传导自然提供足够的热量来加速粒子到地球附近观测到的太阳风通量。与粘度和太阳磁场的稳定效果进行了检查。（验证）
The hydrodynamic equations for the solar corona with no external heat source beyond a thin shell are solved for the case of fast expansion. The corona is assumed to be approximately 10 per cent ionized helium, and the Chapman value for the unihibited thermal conductivity can be used everywhere. The equations are integrated, from the earth to the sun, on an IBM 7090 computer, and a power series expansion is used in the neighborhood of the singularity at r/sub c/, where kT(r/sub c/) = mu/sup 2/(r/sub c/). It is found that thermal conduction naturally supplies sufficient heating to accelerate particles to the observed solar wind flux near the earth, if the inner coronal densities are near the accepted values, with a base temperature near 2 x 10/sup 6/ deg K. The stabilization effects associated with viscosity and the solar magnetic field are examined. (auth)