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高射频活动区域的光谱与太阳耀斑发生之间的相关性
Sara Mulas1, Alberto Pellizzoni2, Marco Marongiu2
1Cagliari Astronomical Observatory, INAF, Via della Scienza 5, 09047, Selargius (CA), Italy. sara.mulas@inaf.it.
Scientific reports
|January 8, 2026
概括
高射频太阳观测可以预测强烈的太阳耀斑. 检测活跃区域的光谱平面化表明,在30小时内发生重大爆发的概率为89%,只有12%的爆发错过了.
科学领域:
- 太阳物理 太阳物理
- 无线电天文学 无线电天文学
- 太空天气 太空天气
背景情况:
- 在过渡区域附近的太阳活跃区域 (ARs) 的磁场对于理解太阳耀斑和冠状质量喷射至关重要.
- 在AR中高磁场强度 (1500-2000G) 导致由于陀螺共振发射的异常亮度光谱.
- 在这些增强的磁场区域观察到高达40%的圆极化.
研究的目的:
- 调查太阳能无线电观测对强烈耀斑事件的预测能力.
- 分析活跃区域的光谱特征与随后的爆发事件之间的相关性.
- 评估基于物理的耀斑预测方法的灵敏度和稳定性.
主要方法:
- 利用来自意大利射电望远镜的K波段频率范围 (18-26 GHz) 在2018-2023年期间捕获的约450张太阳图像.
- 采用太阳能无线电测绘,在活跃区域探测色球磁场.
- 进行了相关性分析,以评估爆发预测方法的性能.
主要成果:
- 在AR中显著检测到光谱平整与30小时内发生强烈爆发的高概率 (约89%) 相相关.
- 大约每周一次的观测节奏在分析的时间间隔内仅错过了大约12%的强烈耀斑.
- 该研究评估了火焰预测技术的灵敏度和稳定性的权衡.
结论:
- 高射频太阳观测为预测强烈太阳耀斑提供了宝贵的工具.
- 在活跃区域中检测光谱平面化是即将发生的能量太阳事件的可靠前体.
- 基于物理的耀斑预测方法表现出有希望的准确性和稳定性,尽管存在观察局限性.
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