Radioastronomical Studies of Plasma Waves in the Solar Corona and Solar Winds

首席研究员（PI）提议解决太阳物理学中一个重要但尚未解决的问题：太阳日冕的加热。他从这样一个假设出发，即这种加热是由磁流体动力学（MHD）波的冕状阻尼引起的，磁流体动力学（MHD）波起源于湍流和光球中磁场的相关波动。计划进行两个实验，这两个实验都是利用MHD波对星系外无线电波的影响，当它们穿过太阳日冕和非常接近太阳的太阳风时。在第一个实验中，PI将通过太阳日冕的湍流等离子体测量射电源的角展宽，并试图获得湍流的空间功率谱信息。在第二个实验中，PI将观测河外射电源，以测量法拉第旋转，这是由于太阳日冕的密度和磁场不规则造成的。这个实验将是Hollwer等人对太阳神号航天器发射机发射的无线电信号观测的延伸。

The Principal Investigator (PI) proposes to address an important, yet unsolved problem in solar physics: the heating of the solar carona. He starts from the assumption that this heating is caused by the damping in the carona of magnetohydrodynamic (MHD) waves, which start from turbulence and the associated fluctuations of magnetic fields in the photosphere. Two experiments are planned, both of which make use of effects that the MHD waves have on extragalactic radio waves as they pass through the solar corona and the solar wind very close to the sun. In the first experiment, the PI will measure angular broadening of radio sources viewed through the solar corona's turbulent plasma and attempt to obtain information on the spatial power spectrum of the turbulence. In the second experiment, the PI will observe extragalactic radio sources to measure Faraday rotation that are due to the density and magnetic field irregularities in the solar corona. This experiment will be an extension of observations by Hollwer et al. of radio signals emitted by the Helios spacecraft transmitter.