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首页> 外文期刊>Plasma physics and controlled fusion >Why is the Sun's corona so hot? Views from SOHO, Yohkoh and solar eclipses
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Why is the Sun's corona so hot? Views from SOHO, Yohkoh and solar eclipses

机译：为什么太阳的日冕这么热？ SOHO，Yohkoh和日食的风景

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It has been known for over 50 years that the outer atmosphere of the Sun, the so-called corona, has a temperature of 10(6) K (similar to 0.1 keV) yet the exact reasons for this are still being debated. The magnetic field that pervades the corona is certainly the source of the heating, but the question is whether the field energy is dissipated via numerous, small, random reconnections (known as 'nanoflares', i.e. small energy releases of about 10(16) J) or the damping of magnetohydrodynamic (MHD) waves propagating up from the Sun's surface layers (the photosphere). Some new evidence from the SOHO and Yohkoh spacecraft, with instruments on board which image the Sun in the extreme ultraviolet and soft x-rays, are shedding new light on the problem-it appears that the energy spectrum of small flare-like phenomena may be such that nanoflares are sufficiently numerous to supply the corona's energy requirements. However, these new findings do not preclude the possibility of MHD wave motions also supplying significant amounts of energy. Theory suggests very short period (<1 s) MHD waves are implicated in the heating process if so. Searches during total solar eclipses for modulations of the white-light coronal intensity that may result are being made with increasingly sophisticated equipment. Some very fast imaging systems are now available, and a description is given of a charge-coupled device camera experiment conducted successfully during the recent total solar eclipse visible in Europe. [References: 19]
机译：50多年来，人们已经知道，太阳的外部大气（所谓的电晕）的温度为10（6）K（约等于0.1 keV），但其确切原因仍在争论中。遍布电晕的磁场当然是加热的来源，但问题是场能量是否通过大量，小的，随机的重新连接（称为“ nanoflares”）消散，即小能量释放约10（16）J ）或从太阳表层（光球）传播的磁流体动力学（MHD）波的阻尼。 SOHO和Yohkoh航天器的一些新证据，带有在极端紫外线和柔和X射线下成像太阳的仪器，正在为这个问题提供新的亮点-看来，类似小耀斑现象的能谱可能是这样，纳米火炬足以提供电晕的能量需求。但是，这些新发现并不排除MHD波动也提供大量能量的可能性。理论表明，加热过程中会牵涉非常短的时间（<1 s）MHD波。在日全食期间搜寻可能会导致白光日冕强度发生变化的设备越来越复杂。现在可以使用一些非常快速的成像系统，并描述了在欧洲最近发生的日全食期间成功进行的电荷耦合器件相机实验。 [参考：19]

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