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The Class of Type III-L Solar Radio Bursts and Their Associations with Solar Energetic Proton Events.

机译：III-L型太阳射电爆炸的类别及其与太阳能质子事件的关系。

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摘要

The source protons of Solar Energetic particle Proton events (defined as "SEP" events for this research) not associated with the Coronal Mass Ejection (CME) shock front are thought to come from either the flare site or the reconnection region beneath the CME. The Type III-L, a new class of solar radio burst has been defined by Cane et al. (2002) and MacDowall et al. (2003) as a sub-set of the Type III burst, beginning after the onset of the soft X-ray (SXR) flare, is long lasting and extends down to at least 1 MHz. The emission source region of Type III-Ls is believed to be at the reconnection region beneath the CME or on the flanks of the CME. Past association studies between SEP events and Type III-Ls began with a biased SEP-selected sample set to see if there can be found support for the emission source region of Type III-Ls and SEPs to come from the same accelerator site at the reconnection region beneath the CME. Unlike previous studies using an SEP-selected sample, I find that when using a radio-selected sample for well-connected SEP events with a solar source in the western hemisphere, the majority of the Type III-L events are associated with SEP events, but not all, and that Type III-L events associated with M- and X- class SXR flares, do not appear to be better predictors of SEP events than do Type II bursts which are associated with the CME shock. Also, I find that the occurrence of Type II events in the radio spectra of SEPs is just as common as the occurrence of Type III-Ls. This indicates that Type III-Ls should not be used as a predictor for SEP events, that the emission source region of Type III-Ls might not be at the reconnection region beneath the CME and reduces the strength of the support found by previous SEP-Type III-L association studies, that the source protons for SEP events necessarily come from the reconnection region beneath the CME. I found that Type III-L events have no strong longitude preference, but SEP events do have a 60% preference between W30 and W90 solar longitude. New data from new long wavelength arrays will help with position mapping the emission source regions of Type III-L bursts. An investigation was done on the internal structure of Type III-Ls. An implication of the result that the separation between components of the Type III-L burst was found to be longer than the separation between the components of Impulsive-Phase Type IIIs (defined as "Imp-Type IIIs"), is that the duration of the Type III-L components appears to be longer than those of Imp-Type IIIs. The result that the components of the Imp-Type IIIs have a faster frequency-time drift-rate than those of the Type III-Ls, shows that the source electrons for the Imp-Type IIIs appear to have a faster source emission velocity than do Type III-Ls. This is understandable as the source electrons for the Imp-Type IIIs are thought to come directly from the active region flare site, whereas the source electrons for Type III-Ls have a longer path along the neutral current sheet to either the reconnection region beneath the CME or up to the flanks of the CME. This gives us a reason as to why the Type III-L emission is delayed in respect to the Imp-Type IIIs. With their energy decreased, these Type III-L source electrons would form emission with a source velocity and frequency-time drift-rate slower than that of the Imp-Type IIIs. Data with better time and frequency resolution should help determine if there are additional weaker Type III-L components. Timing studies between SXR flares, the expansion of CMEs and the evolution of Type III-L components, should determine if electron accelerator sites for the Type III-L components are at a reconnection region beneath the CME or on the flanks of the CME.
机译：与日冕质量抛射（CME）激波锋无关的太阳高能粒子质子事件（在本研究中定义为“ SEP”事件）的源质子被认为来自火炬站点或CME下方的重新连接区域。 Cane等人已经定义了III-L型，一种新型的太阳无线电脉冲串。 （2002）和MacDowall等。 （2003年）作为III型爆发的子集，它在软X射线（SXR）耀斑爆发后开始，持续时间长，并向下延伸至至少1 MHz。 III-L型发射源区域被认为位于CME下方或CME侧面的重新连接区域。 SEP事件与III-L型之间过去的关联研究始于有偏倚的SEP选择的样本集，以查看是否可以找到对III-L型和SEP排放源区域的支持来自重新连接时的同一加速器位置芝商所下方的区域。与以前使用SEP选定样本进行的研究不同，我发现当使用无线电选出的样本对西半球与太阳能有良好联系的SEP事件进行分析时，大多数III-L型事件与SEP事件有关，但并非全部，与M级和X级SXR耀斑相关的III-L型事件似乎不比与CME休克相关的II型爆发更好地预测SEP事件。另外，我发现在SEP的无线电频谱中II型事件的发生与III-L型事件的发生一样普遍。这表明III-L型不应该用作SEP事件的预测指标，III-Ls型的发射源区域可能不在CME下方的重新连接区域，从而降低了先前SEP-L发现的支撑强度。 III-L型关联研究表明，SEP事件的质子必定来自CME下方的重新连接区域。我发现III-L型事件没有强的经度偏爱，但是SEP事件在W30和W90的太阳经度之间确实有60％的偏爱。来自新的长波长阵列的新数据将有助于对III-L型猝发的发射源区域进行位置映射。对III-L型的内部结构进行了调查。结果表明，发现III-L型脉冲串之间的间隔比脉冲型IIIs分量（定义为“ Imp-Type IIIs”）之间的间隔更长，是因为持续时间为III-L型组件似乎比Imp-III型组件更长。 Imp-Type III的组件具有比III-Ls更快的频率-时间漂移率，结果表明Imp-Type IIIs的源电子似乎具有比其快的源发射速度。 III-L型。这是可以理解的，因为Imp-Type III的源电子被认为直接来自有源区的光斑，而III-Ls的源电子沿着中性点电流板到达位于其下方的重新连接区的路径更长。 CME或直至CME的侧面。这为我们提供了一个理由，说明为什么相对于Imp-III型，III-L型发射延迟了。随着能量的减少，这些III-L型源电子将形成发射，其源速度和频率-时间漂移率比Imp-III型慢。具有更好的时间和频率分辨率的数据应有助于确定是否还有其他较弱的III-L型分量。 SXR耀斑之间的计时研究，CME的膨胀以及III-L型组分的演变，应确定III-L型组分的电子促进剂位点是在CME下方还是CME侧面的重连接区。

著录项

  • 作者

    Duffin, Robert Thomas.;

  • 作者单位

    George Mason University.;

  • 授予单位 George Mason University.;
  • 学科 Physics Astrophysics.;Physics Fluid and Plasma.;Physics Astronomy and Astrophysics.
  • 学位 Ph.D.
  • 年度 2011
  • 页码 154 p.
  • 总页数 154
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

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