SOLAR SOURCES OF 3He-RICH SOLAR ENERGETIC PARTICLE EVENTS IN SOLAR CYCLE 24
SOLAR SOURCES OF 3He-RICH SOLAR ENERGETIC PARTICLE EVENTS IN SOLAR CYCLE 24
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DOI：
10.1088/0004-637x/806/2/235
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发表时间：
2015-05
期刊：
影响因子：
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通讯作者：
N. Nitta;G. Mason;Linghua Wang;C. Cohen;M. Wiedenbeck
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作者：
N. Nitta;G. Mason;Linghua Wang;C. Cohen;M. Wiedenbeck
使用太阳动力学天文台上的大气成像组件（AIA）获得的高节奏 EUV 图像，我们研究了 26 个 ≲1 MeV 核子−1 处富含 3He 的太阳高能粒子事件的太阳源，这些事件在太阳周期 24 期间被高级成分探测器很好地观测到。太阳源的识别是基于富含 3He 事件与 Wind 观测到的 III 型射电爆发和电子事件的关联。太阳与地球关系观测站的 EUV 图像进一步验证了源位置，该图像提供了从地球上看不到的区域的太阳活动信息。根据AIA的观测，富含3He的事件不仅与太阳周期23研究中强调的日冕喷流有关，而且还与更广泛的空间喷发有关。富含 3He 事件的特性似乎与源区的特性没有很强的相关性。与之前的研究一样，简单的势场源表面模型与帕克螺旋相结合并不总是能够充分再现源区域和观察者之间的磁连接。相反，我们发现源区的广泛纵向分布远远超出了西翼，其经度与观测到的太阳风速的预期显着偏离。
Using high-cadence EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, we investigate the solar sources of 26 3He-rich solar energetic particle events at ≲1 MeV nucleon−1 that were well-observed by the Advanced Composition Explorer during solar cycle 24. Identification of the solar sources is based on the association of 3He-rich events with type III radio bursts and electron events as observed by Wind. The source locations are further verified in EUV images from the Solar and Terrestrial Relations Observatory, which provides information on solar activities in the regions not visible from the Earth. Based on AIA observations, 3He-rich events are not only associated with coronal jets as emphasized in solar cycle 23 studies, but also with more spatially extended eruptions. The properties of the 3He-rich events do not appear to be strongly correlated with those of the source regions. As in the previous studies, the magnetic connection between the source region and the observer is not always reproduced adequately by the simple potential field source surface model combined with the Parker spiral. Instead, we find a broad longitudinal distribution of the source regions extending well beyond the west limb, with the longitude deviating significantly from that expected from the observed solar wind speed.