The sun has hurled plasma and other magnetic activity toward the Earth.

太阳向地球发射了等离子体并进行了其他磁活动。

As this plasma slowly swirls, it creates areas of intense magnetic activity called sunspots.

当这种等离子体缓慢旋转时，它会产生称为太阳黑子的强烈磁场活动区域。

This ongoing movement can produce temporary concentrations of magnetic activity which inhibit the movement of molecules and in turn reduce heat in that area.

这一持续发生的运动能暂时将磁场活动集中变强，从而抑制该区域的分子活动，导致温度降低。

But unlike the stable charged particles that maintain magnetic activity on Earth, this plasma is constantly in flux, alternately disrupting and amplifying the sun's magnetic field.

但不像地球上由稳定的带电粒子所形成的稳定的磁场，这些等离子体持续处于流通状态，交替扰乱并放大太阳的磁场。

This kind of detail offered a real-time indication of the sun's magnetic activity, allowing scientists to track all kinds of solar phenomena, including volatile solar flares.

这个级别的细节可以实时反应出太阳的磁场活动，从而让科学家能够追踪各种各样的太阳现象，包括爆炸性的太阳耀斑。

After centuries of observing sunspots, researchers have learned the Sun's usual magnetic activity follows an 11-year cycle, giving us a window into when solar storms are most likely to occur.

经过几个世纪对太阳黑子的观察，研究人员了解到太阳通常的磁活动遵循 11 年的周期，这让我们有机会了解太阳风暴最有可能发生的时间。