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首页> 外文期刊>The Astrophysical journal >CATASTROPHIC ERUPTION OF MAGNETIC FLUX ROPE IN THE CORONA AND SOLAR WIND WITH AND WITHOUT MAGNETIC RECONNECTION
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CATASTROPHIC ERUPTION OF MAGNETIC FLUX ROPE IN THE CORONA AND SOLAR WIND WITH AND WITHOUT MAGNETIC RECONNECTION

机译：带有和不带有磁连接的日冕风和日风中的磁通量的巨泻爆发

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摘要

It is generally believed that the magnetic free energy accumulated in the corona serves as a main energy source for solar explosions such as coronal mass ejections (CMEs). In the framework of the flux rope catastrophe model for CMEs, the energy may be abruptly released either by an ideal magnetohydrodynamic (MHD) catastrophe, which belongs to a global magnetic topological instability of the system, or by a fast magnetic reconnection across preexisting or rapidly developing electric current sheets. Both means of magnetic energy release are thought to be important to CME dynamics. To disentangle their contributions, we construct a flux rope catastrophe model in the corona and solar wind and compare different cases in which we either prohibit or allow magnetic reconnection to take place across rapidly growing current sheets during the eruption. It has been demonstrated that CMEs, even fast ones, can be produced taking the ideal MHD catastrophe as the only process of magnetic energy release. Nevertheless, the eruptive speed can be significantly enhanced after magnetic reconnection sets in. In addition, a smooth transition from slow to fast eruptions is observed when increasing the strength of the background magnetic field, simply because in a stronger field there is more free magnetic energy at the catastrophic point available to be released during an eruption. This suggests that fast and slow CMEs may have an identical driving mechanism.
机译：通常认为，电晕中积累的磁自由能是太阳爆炸（如日冕物质抛射（CME））的主要能源。在CME的通量绳巨灾模型的框架中，能量可能由于理想的磁流体动力学（MHD）巨灾而突然释放，MHD巨灾属于系统的整体磁拓扑不稳定性，也可能是通过预先存在或快速跨越的快速磁重新连接而释放的开发电流表。两种释放磁能的方式都被认为对CME动力学很重要。为了弄清它们的作用，我们在日冕和太阳风中构造了一个磁通绳突变模型，并比较了在喷发过程中禁止或允许在迅速增长的电流层上进行磁重新连接的不同情况。已经证明，以理想的MHD灾难为唯一的磁能释放过程，可以生产CME，甚至是快速的CME。尽管如此，在重新建立磁连接后，喷发速度可以得到显着提高。此外，当增加背景磁场的强度时，可以观察到从慢喷发到快速喷发的平稳过渡，这仅仅是因为在更强的磁场中存在更多的自由磁能在爆发时可释放的灾难点。这表明快速和慢速CME可能具有相同的驱动机制。

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  • 来源
    《The Astrophysical journal》 |2007年第2pt1期|1421-1427|共7页
  • 作者

    Y. Chen; Y. Q. Hu; S. J. Sun;

  • 作者单位

    Department of Space Science and Applied Physics, Shandong University at Weihai, Weihai Shandong, 264209 China;

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  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
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  • 入库时间 2022-08-18 01:48:58

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