Relationship of peak fluxes of solar radio bursts and X-ray class of solar flares: Application to early great solar flares

IF 2.2 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Keitarou Matsumoto, Satoshi Masuda, Masumi Shimojo, Hisashi Hayakawa
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引用次数: 1

Abstract

Abstract Large solar flares occasionally trigger significant space-weather disturbances that affect the technological infrastructures of modern civilization, and therefore require further investigation. Although these solar flares have been monitored by satellite observations since the 1970s, large solar flares occur only infrequently and restrict systematic statistical research owing to data limitations. However, Toyokawa Observatory has operated solar radio observations at low frequencies (at 3.75 and 9.4 GHz) since 1951 and captured the early great flares as solar radio bursts. To estimate the magnitudes of flares that occurred before the start of solar X-ray (SXR) observations with the Geostationary Operational Environmental Satellite (GOES) satellites, we show the relationship between microwave fluxes at 3.75 and 9.4 GHz and X-ray fluxes of flares that occurred after 1988. In total, we explored 341 solar flares observed with the Nobeyama Radio Polarimeters and Toyokawa Observatory from 1988–2014 and compared them with the SXR observations recorded by the GOES satellites. The correlation coefficient was approximately 0.7. Therefore, the GOES X-ray class can be estimated from the peak flux at 3.75 and 9.4 GHz with a large variance and an error of factor of 3 (1σ). Thus, for the first time, we quantitatively estimated the light curves of two early solar flares observed in 1956 February by the Toyokawa solar radio observations using the relationship between SXR thermal radiation and microwave nonthermal radiation (Neupert, 1968, ApJ, 153, 59).
太阳射电暴峰值通量与太阳耀斑x射线等级的关系:早期大太阳耀斑的应用
大型太阳耀斑偶尔会引发重大的空间天气干扰,影响现代文明的技术基础设施,因此需要进一步研究。虽然这些太阳耀斑自1970年代以来一直通过卫星观测进行监测,但由于数据的限制,大型太阳耀斑很少发生,并限制了系统的统计研究。然而,自1951年以来,东川天文台一直在低频率(3.75 GHz和9.4 GHz)上进行太阳射电观测,并捕捉到了早期的太阳射电爆发大耀斑。为了估计在地球同步运行环境卫星(GOES)开始太阳x射线(SXR)观测之前发生的耀斑的大小,我们展示了3.75和9.4 GHz的微波通量与1988年后发生的耀斑的x射线通量之间的关系。我们研究了Nobeyama射电偏振计和Toyokawa天文台在1988-2014年间观测到的341个太阳耀斑,并将它们与GOES卫星记录的SXR观测结果进行了比较。相关系数约为0.7。因此,从3.75 GHz和9.4 GHz的峰值通量可以估计出GOES的x射线类别,方差较大,误差为3 (1σ)。因此,我们首次利用SXR热辐射和微波非热辐射之间的关系,定量估计了1956年2月Toyokawa太阳射电观测观测到的两个早期太阳耀斑的光曲线(Neupert, 1968, ApJ, 153,59)。
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来源期刊
Publications of the Astronomical Society of Japan
Publications of the Astronomical Society of Japan 地学天文-天文与天体物理
CiteScore
4.10
自引率
13.00%
发文量
98
审稿时长
4-8 weeks
期刊介绍: Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.
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