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Energy release in the solar corona from spatially resolved magnetic braids

机译:空间分解的磁性辫子在太阳日冕中释放能量

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摘要

It is now apparent that there are at least two heating mechanisms in the Sun's outer atmosphere, or corona. Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000 K (refs 1-3). The active corona needs additional heating to reach 2,000,000-4,000,000 K; this heat has been theoretically proposed to come from the reconnection and unravelling of magnetic 'braids'. Evidence favouring that process has been inferred, but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought to have an angular width of about 0.2 arc seconds have not been resolved~(10,18-20). Fine-scale braiding has been seen~(21.22) in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000 K. Although our 5-minute observations cannot unambiguously identify the field reconnection and subsequent relaxation as the dominant heating mechanism throughout active regions, the energy available from the observed field relaxation in our example is ample for the observed heating.%太阳的外层大气(日冕)比其表面温度高数百万rn度。寻找能够将能量从太阳内部以这样大的规rn模转移到周边的机制的工作已识别出两个可信rn度很高的候选机制:波加热作用被认为将日冕rn加热到15075K;同时“磁辫子”的重新连接和rn拆开也被提出是将温度升高到接近40075K的rn机制。搭载在一个探空火箭上的一台高分辨率rn照相机所获得的5分钟长的系列图像,提供了rn支持后一个机制的新证据。这些图像显示,在rn一个日冕活跃区域存在分辨率达到约150公里rn的精细尺度的结辫现象,而且这些图像也与足rn以产生所观测到的加热现象的能量生成(过程)rn相致。
机译:现在很明显,在太阳的外部大气或电晕中至少存在两种​​加热机制。在安静的太阳时段,波浪加热可能是普遍的机制,并且可能有助于将电晕加热到1,500,000 K(参考1-3)。活性电晕需要额外加热以达到2,000,000-4,000,000 K;从理论上讲,这种热量来自磁性“编织层”的重新连接和散开。已经推断出支持该过程的证据,但尚未得到普遍接受,因为观测稀疏,并且通常来说,被认为具有约0.2弧秒的角宽度的编织磁链尚未解决〜(10,18- 20)。在色球层中已经观察到精细的编织(21.22),但是直到现在为止,在电晕中都没有看到。在这里,我们报告以0.2弧秒的分辨率观测到的日冕活动区域中的磁编织带,它们重新连接,放松并耗散了足够的能量以将结构加热到约4,000,000K。尽管我们5分钟的观测无法明确地确定磁场重新连接和随后的弛豫是整个活动区域的主要加热机制,在我们的示例中,观察到的场弛豫可提供的能量对于所观察到的加热是足够的。%太阳的外层大气(日冕)比其表面温度高数百万rn度。寻找能够将能量从太阳内部以这样的大规规模转移到周围的机制的工作已识别出两个可信rn度很高的替代机制:波加热作用被认为将日冕rn加热到15075K;同时“磁能子”的重新连接和rn拆开也被提出是将温度升高到接近40075K的rn机制。搭载在一个探空火箭上的一台高温rn照相机所获得的5分钟长的系列图像这些图像显示,在rn一个日冕活动区域存在分辨率达到约150 kmrn的精细尺度的结弱现象,而且这些图像也与足rn以产生所观察到的加热现象的能量生成(过程)rn相致。

著录项

  • 来源
    《Nature》 |2013年第7433期|501-503a3|共4页
  • 作者单位

    Marshall Space Flight Center, NASA, Mail CodeZP13, MSFC, Alabama 36812, USA;

    Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 01238, USA;

    Marshall Space Flight Center, NASA, Mail CodeZP13, MSFC, Alabama 36812, USA;

    Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Palo Alto, California 94304, USA;

    Center for Space and Aeronautic Research, University of Alabama-Huntsville, 320 Sparkman Avenue, Huntsville, Alabama 35812, USA;

    Marshall Space Flight Center, NASA, Mail CodeZP13, MSFC, Alabama 36812, USA;

    Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 01238, USA;

    Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 01238, USA;

    Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 01238, USA;

    Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 01238, USA;

    Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Palo Alto, California 94304, USA;

    Lebedev Physical Institute, 53 Leninski Prospekt, 119991 Moscow, Russia;

    Southwest Research Institute, Instrumentation and Space Research Division, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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  • 正文语种 eng
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