Nat Gopalswamy, Pertti Mäkelä, Sachiko Akiyama, Hong Xie, Seiji Yashiro, Stuart D. Bale, Robert F. Wimmer-Schweingruber, Patrick Kühl, Säm Krucker
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SolO’s Spectrometer Telescope for Imaging X-rays (STIX) imaged an intense (X3.3) flare, which occurred ≈ 41° behind the east limb, from heliographic coordinates S13E131. Forward modeling of the coronal mass ejection (CME) flux rope revealed that it impulsively accelerated (3.54 km s<sup>−2</sup>) to attain a peak speed of 2162 km s<sup>−1</sup>. SolO’s energetic particle detectors (EPD) observed protons up to ≈ 1 GeV from the extended shock and electrons that produced a complex type II burst and possibly type III bursts. The durations of SGRE and type II burst are consistent with the linear relation between these quantities obtained from longer duration (> 3 hours) SGRE events. All these observations are consistent with an extended shock surrounding the CME flux rope, which is the likely source of high-energy protons required for the SGRE event. 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引用次数: 0
摘要
我们报告了2024年9月9日费米卫星上的大面积望远镜(LAT)观测到的持续伽马射线发射(SGRE)事件。该事件与太阳背面爆发有关,由多个航天器观测到,如太阳和日光层天文台(SOHO)、日地关系天文台(STEREO)、帕克太阳探测器(PSP)、太阳轨道器(SolO)、太阳动力学天文台(SDO)、Wind和GOES,以及地面射电望远镜。费米/LAT观测了从太阳背面喷发出来的EUV波穿过边缘到达太阳正面后的SGRE。SolO的x射线成像光谱仪望远镜(STIX)拍摄到了一个强烈的(X3.3)耀斑,它发生在东翼后约41°,位于日冕坐标S13E131处。日冕物质抛射(CME)通量绳的正演模拟显示,它的脉冲加速(3.54 km s−2)达到了2162 km s−1的峰值速度。SolO的高能粒子探测器(EPD)从扩展激波中观测到高达≈1 GeV的质子和电子,产生了复杂的II型爆发,也可能是III型爆发。SGRE和II型爆发的持续时间与从持续时间较长的SGRE事件(>; 3小时)中获得的数量之间的线性关系是一致的。所有这些观测结果都与围绕CME通量绳的延伸激波相一致,这可能是SGRE事件所需的高能质子的来源。我们将这次事件与其他六次SGRE后肢喷发(BTL)进行了比较,发现它们都与高能冲击驱动的cme一致。我们还发现在BTL源位置有明显的东西不对称(3:1)。
Multispacecraft Observations of the 2024 September 9 Backside Solar Eruption That Resulted in a Sustained Gamma Ray Emission Event
We report on the 2024 September 9 sustained gamma-ray emission (SGRE) event observed by the Large Area Telescope (LAT) on board the Fermi satellite. The hevent was associated with a backside solar eruption observed by multiple spacecraft such as the Solar and Heliospheric Observatory (SOHO), Solar Terrestrial Relations Observatory (STEREO), Parker Solar Probe (PSP), Solar Orbiter (SolO), Solar Dynamics Observatory (SDO), Wind, and GOES, and by ground-based radio telescopes. Fermi/LAT observed the SGRE after the EUV wave from the backside eruption crossed the limb to the frontside of the Sun. SolO’s Spectrometer Telescope for Imaging X-rays (STIX) imaged an intense (X3.3) flare, which occurred ≈ 41° behind the east limb, from heliographic coordinates S13E131. Forward modeling of the coronal mass ejection (CME) flux rope revealed that it impulsively accelerated (3.54 km s−2) to attain a peak speed of 2162 km s−1. SolO’s energetic particle detectors (EPD) observed protons up to ≈ 1 GeV from the extended shock and electrons that produced a complex type II burst and possibly type III bursts. The durations of SGRE and type II burst are consistent with the linear relation between these quantities obtained from longer duration (> 3 hours) SGRE events. All these observations are consistent with an extended shock surrounding the CME flux rope, which is the likely source of high-energy protons required for the SGRE event. We compare this event with six other behind-the-limb (BTL) SGRE eruptions and find that they are all consistent with energetic shock-driving CMEs. We also find a significant east-west asymmetry (3:1) in the BTL source locations.
期刊介绍:
Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.