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A comparative analysis on two solar proton events

Chinese Science Bulletin 2007年第1期52卷 47-51页

作者： le guiming1,2,3.4, han yanben2 & zhang yijun3.1 key laboratory of radiometric calibration and validation for environmental satellites,{3., Beijing 100081, china 2 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, china 3.Chinese Academy of meteorological Sciences,{3., Beijing 100081, china 4 National Center for Space Weather,{3., Beijing 100081, china key laboratory of radiometric {3. and {3. for environmental satellites China Meteorological Administration Beijing China National Astronomical Observatoires Chinese Academy of Sciences Beijing China Chinese Academy of meteorological Sciences China Meteorological Administration Beijing China

This paper presents a comparative analysis on the two Solar Proton Events (SPE), which occurred on 14 July 2000 (Bastille Day) and 28 October 2003.(28OCT03. respectively. It is found that although the peak flux of the latter seemed to be greater than that of the former based on geostationary observations, the maximum intensities of the energetic protons (>10 MeV and 3. MeV) during the Bastille Day event were all higher than those of the 28OCT03.event according to the interplanetary observations. Further analysis indicated that the quantity of the seed particles, which could be accelerated to the energies exceeding 10 and 3. MeV by the Coronal Mass Ejection (CME)-driven shock on 14 July 2000, was far larger than that of the 28OCT03.event. In the Bastille Day case, when the CME approached to the height around 14 R⊙, the CME-driven shock would reach its maximum capacity in accelerating the solar en- ergetic protons (>100 MeV). In contrast, on 28 October 2003. when CME approached to the height about 58R⊙, the CME-driven shock reached its highest potential in accelerating the solar energetic protons of the same category. At this moment, the peak flux (>100 MeV) was about 155 pfu, which was much lower than 3.5 pfu measured on 14 July 2000. This demonstrated that in the Bastille Day event, the quantity of the seed particles, which could be accelerated to the energy beyond 100 MeV, was significantly larger than its counterpart in the 28OCT03.case. Therefore, the peak flux of an SPE event depends not only on the interplanetary intensity of the solar energetic particles, but also on the velocity of the associated CME-driven shock, and the quantity of the seed particles as well as on the interplanetary magnetic en- vironment. This paper also reveals that the magnetic sheath associated with ICME on 28 October 2003.captured a large number of solar energetic protons, including those having energy greater than 100 MeV.

关键词：太阳质子 CME 太阳耀斑太阳系

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Solar release time of solar energetic particles and associated acceleration source in corona

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Chinese Science Bulletin 2008年第2期53卷 161-168页

作者： le guiming1,2,3.4, TANG YuHua1 & han {3.4 1 Department of Astronomy, Nanjing University, Nanjing 210093.{3. 2 key laboratory of radiometric calibration and validation for environmental satellites, china meteorological administration, Beijing 100081,{3. 3.National Center for Space Weather, china meteorological administration, Beijing 100081,{3. 4 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012,{3. Department of Astronomy Nanjing University Nanjing China key laboratory of radiometric {3. and {3. for environmental satellites China Meteorological Administration Beijing China National Center for Space Weather China Meteorological Administration Beijing China National Astronomical Observatories Chinese Academy of Sciences Beijing China

Solar energetic particles (SEPs) are accelerated in corona at an early phase of solar energetic particle events (SEPE). The acceleration mechanism of SEPs in corona can only be inferred from an analysis of multi-band observational data, as the observation of SEPs is usually made around 1AU. In this context, people have investigated spectrums, charge state, solar release time (SRT), and multi-band data of SEPEs, in an attempt to judge the acceleration mechanism of SEPs. The SRT computation of SEPs is an important and commonly used approach to study the acceleration mechanism of SEPs in corona. This paper reviews some important findings concerning the SRT computation of SEPs, and analyzes different merits of each approach for such calculation, based on a range of SEPE case studies. This paper also analyzes and discusses both possible and actual acceleration mechanisms of a number of SEPEs, by calculating the SRT of the SEPEs. Finally, the paper summarizes the possible problems in studying an acceleration mechanism of SEPEs inferred from the SRT of SEP.

关键词：阳光释放时间加速度电晕太阳耀斑

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