Rust D M
The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723-6099, USA.
Adv Space Res. 1992;12(2-3):289-301. doi: 10.1016/0273-1177(92)90119-i.
This is a survey of solar phenomena and physical models that may be useful for improving forecasts of solar flares and proton storms in interplanetary space. Knowledge of the physical processes that accelerate protons has advanced because of gamma-ray and X-ray observations from the Solar Maximum Mission telescopes. Protons are accelerated at the onset of flares, but the duration of any subsequent proton storm at 1 AU depends on the structure of the interplanetary fields. X-ray images of the solar corona show possible fast proton escape paths. Magnetographs and high-resolution visible-band images show the magnetic field structure near the acceleration region and the heating effects of sunward-directed protons. Preflare magnetic field growth and shear may be the most important clues to the physical processes that generate high energy solar particles. Any dramatic improvement in flare forecasts will require high resolution solar telescopes in space. Several possibilities for improvements in the art of flare forecasting are presented, among them: the use of acoustic tomography to probe for subsurface magnetic fields; a satellite-borne solar magnetograph; and an X-ray telescope to monitor the corona for eruptions.
这是一项对太阳现象和物理模型的调查，这些现象和模型可能有助于改进对太阳耀斑和行星际空间中质子风暴的预测。由于太阳极大期任务望远镜的伽马射线和X射线观测，对质子加速物理过程的认识有了进展。质子在耀斑开始时被加速，但随后在1天文单位处任何质子风暴的持续时间取决于行星际磁场的结构。日冕的X射线图像显示了可能的快速质子逃逸路径。磁强计和高分辨率可见波段图像显示了加速区域附近的磁场结构以及向日质子的加热效应。耀斑前磁场的增长和剪切可能是产生高能太阳粒子的物理过程的最重要线索。耀斑预测的任何显著改进都将需要太空的高分辨率太阳望远镜。文中提出了几种改进耀斑预测技术的可能性，其中包括：使用声学层析成像探测地下磁场；卫星搭载的太阳磁强计；以及用于监测日冕爆发的X射线望远镜。
