Science. 1985 Apr 5;228(4695):9-15. doi: 10.1126/science.228.4695.9.
High-resolution microwave observations are providing new insights into the nature of active regions and eruptions on the sun and nearby stars. The strength, evolution, and structure of magnetic fields in coronal loops can be determined by multiple-wavelength observations with the Very Large Array. Flare models can be tested with Very Large Array snapshot maps, which have angular resolutions of better than 1 second of arc in time periods as short as 10 seconds. Magnetic changes that precede solar eruptions on time scales of tens of minutes involve primarily emerging coronal loops and the interactions of two or more loops. Magnetic reconnection at the interface of two closed loops may accelerate electrons and trigger the release of microwave energy in the coronal parts of the magnetic loops. Nearby main-sequence stars of late spectral type emit slowly varying microwave radiation and stellar microwave bursts that show striking similarities to those of the sun.
高分辨率微波观测为太阳和附近恒星活动区和爆发的本质提供了新的认识。甚大阵的多波长观测可以确定日冕环中磁场的强度、演化和结构。甚大阵的快照图可以用来测试耀斑模型，其在 10 秒的时间内具有优于 1 秒弧的角分辨率。在数十分钟的时间尺度上，太阳爆发前的磁变化主要涉及新出现的日冕环和两个或多个环的相互作用。两个闭合环界面上的磁重联可能会加速电子，并触发磁环日冕部分释放微波能量。晚型主序星发出缓慢变化的微波辐射和恒星微波爆发，与太阳的辐射和爆发非常相似。
