Energetic particle observations from the Ulysses COSPIN instruments obtained during the October–November 2003 events
Energetic particle observations from the Ulysses COSPIN instruments obtained during the October–November 2003 events
复制标题
Ulysses COSPIN 仪器在 2003 年 10 月至 11 月事件期间获得的高能粒子观测结果
DOI：
--
复制
发表时间：
2005
期刊：
影响因子：
--
通讯作者：
Ming Zhang
中科院分区：
文献类型：
--
作者：
R. B. Mckibben;J. Anglin;J. J. Connell;S. Dalla;B. Heber;H. Kunow;C. Lopate;R. Marsden;T. Sanderson;Ming Zhang
[1]我们报道了在2003年10月/11月的强烈太阳活动期间，Ulysses航天器上的六台Ulysses COSPIN高能带电粒子仪器对从0.3 MeV到>；100 MeV能量范围内的太阳高能粒子强度的综合观测。我们还讨论了由这些仪器在选定的能量范围内对粒子各向异性的观测。Ulysses位于木星轨道附近，仅在太阳赤道平面以北约6°处，它提供了重要的测量结果，以便与1 AU的观测结果进行比较，并评估在太阳活动周期衰退期这段孤立但强烈的太阳活动期间粒子传播的性质。最重要的结论是，在整个事件过程中，内日光层中的粒子数量高度不均匀，受到太阳风中的流界面等磁性结构的强烈引导和限制。这与太阳周期高峰期附近的大事件后迅速建立的几乎一致的强度形成了强烈的对比。特别感兴趣的是(1)可能在5.2AU观测到通量管的不同填充，并在源传播过程中将高能(>；∼20 MeV)粒子限制在通量管中；(2)大型日冕物质抛射(CME)内部明显排除高能粒子；(3)通过与同一CME的相互作用，可能从木星触发电子释放，以及电子在CME闭合场内的传播。
[1] We report comprehensive observations of solar energetic particle intensities at energies from 0.3 to >100 MeV made by the suite of six Ulysses COSPIN energetic charged particle instruments on the Ulysses spacecraft during the period of intense solar activity in October/November 2003. We also discuss observations of particle anisotropies in selected energy ranges made by these instruments. Located near the orbit of Jupiter and only about 6° north of the heliographic equatorial plane, Ulysses provided important measurements for comparison with 1 AU observations and for assessing the nature of particle propagation in this period of isolated but intense solar activity in the declining phase of the solar activity cycle. The most significant conclusion is that the particle populations in the inner heliosphere were highly nonuniform throughout the events, strongly guided and confined by magnetic structures such as stream interfaces in the solar wind. This provides strong contrast to the nearly uniform intensities that were quickly established after large events near the peak of the solar cycle. Points of particular interest are (1) possible observation at 5.2 AU during onset of differential filling of flux tubes and confinement of high-energy (>∼20 MeV) particles to flux tubes in the course of propagation from the source; (2) apparent exclusion of energetic particles from the interior of a large coronal mass ejection (CME); (3) possible triggered release of electrons from Jupiter by interaction with the same CME, and propagation of the electrons within the closed fields of the CME.