Spectra and anisotropy of cosmic rays during gle64

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Abstract

Ground-based observations of cosmic rays by the spectrographic global survey method were used to study the ground-level enhancement in cosmic ray intensity on August 24, 2002. Spectra of variations of primary cosmic rays and their anisotropy were obtained. Based on measurements from the GOES spacecraft and global network of cosmic ray stations, the differential rigidity spectra of accelerated particles in the vicinity of the Sun were calculated. The maximum rigidity to which solar particles were accelerated was estimated.

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About the authors

I. I. Kovalev

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences

Author for correspondence.
Email: ivankov@iszf.irk.ru
Russian Federation, Irkutsk

M. V. Kravtsova

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences

Email: rina@iszf.irk.ru
Russian Federation, Irkutsk

S. V. Olemskoy

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences

Email: osv@iszf.irk.ru
Russian Federation, Irkutsk

V. E. Sdobnov

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences

Email: sdobnov@iszf.irk.ru
Russian Federation, Irkutsk

References

  1. Белов А.В., Ерошенко Е.А., Крякунова О.Н., Курт В.Г., Янке В.Г. Наземные возрастания солнечных космических лучей в трех последних циклах солнечной активности // Геомагнетизм и аэрономия. Т. 50. №1. С. 23—36. 2010.
  2. Дворников В.М., Кравцова М.В., Сдобнов В.Е. Диагностика электромагнитных характеристик межпланетной среды по эффектам в космических лучах // Геомагнетизм и аэрономия. Т. 53. № 4. С. 457—468. 2013. https://doi.org/10.7868/S001679401304007X
  3. Логачёв Ю.И., Базилевская Г.А., Вашенюк Э.В. и др. Каталог солнечных протонных событий 23-го цикла солнечной активности (1996−2008 гг.). ESDBrepository, ГЦ РАН, Москва. https://doi.org/10.2205/ESDB-SAD-P-001-RU
  4. Луковникова А.А., Сдобнов В.Е. Питч-угловая анизотропия и дифференциальные жесткостные спектры космических лучей во время GLE 2 и 6 мая 1998 г. // Солнечно-земная физика. Т. 8. № 2. С. 29—33. 2022. https://doi.org/10.12737/szf-82202204
  5. Dvornikov V.M., Sdobnov V.E. Analyzing the solar proton event of 22 October 1989, using the method of spectrographic global survey // Solar Phys. V. 178. № 2. P. 405—422. 1998.
  6. Gopalswamy N., Xie H., Yashiro S., et al. Properties of ground level enhancement events and the associated solar eruptions during solar cycle 23 // Space Sci. Rev. V. 171. P. 23—60. 2012. https://doi.org/10.1007/s11214-012-9890-4
  7. Kovalev I.I., Olemskoy S.V., Sdobnov V.E. A proposal to extend the spectrographic global survey method // J. Atmosp. Solar-Terr. Phys. V. 235. P. 105887. 2022. https://doi.org/10.1016/j.jastp.2022.105887
  8. Kravtsova M.V., Sdobnov V.E. Cosmic ray ground level enhancement on August 24, 1998 // Bull. Rus. Acad. Sci.: Phys. V. 87. № 7. P. 1018—1020. 2023. https://doi.org/10.3103/S1062873823702428
  9. Lugaz N., Roussev I.I., Sokolov I.V., Jacobs C. The August 24, 2002 coronal mass ejection: when a western limb event connects to earth // Proc. IAU 257 Symposium. P. 391—398. 2009. https://doi.org/10.1017/S1743921309029615
  10. Miroshnichenko L.I. Solar Cosmic rays: fundamentals and applications. Springer, 2014. 521 p.
  11. Miroshnichenko L.I., Yanke V.G. Size distributions of solar proton events: methodological and physical restrictions // Solar Phys. V. 291. P. 3685—3704. 2016. https://doi.org/10.1007/s11207-016-1002-2
  12. Mishev A., Poluianov S., Usoskin I. Assessment of spectral and angular characteristics of sub-GLE events using the global neutron monitor network // J. Space Weather and Space Climate. 7. A28. 2017. https://doi.org/10.1051/swsc/2017026
  13. Papaioannou A., Kouloumvakos A., Mishev A., et al. The first ground level enhancement of solar cycle 25 on 28 October 2021 // Astron. Astrophys. V. 660. L5. 2022. https://doi.org/10.1051/0004-6361/202142855
  14. Raymond J. C., Ciaravella A., Dobrzycka D., et al. Far-ultraviolet spectra of fast coronal mass ejections associated with X-class flares // Astrophys. J. V. 597. № 2. P. 1106—1117. 2003. https://doi.org/10.1086/378663
  15. Struminsky A.B., Logachevb Yu.I., Grigorieva I.Yu., Sadovski A.M. Two types of gradual events: solar protons and relativistic electrons // Geomag. Aeron. V. 60. № 8. P. 1057—1066. 2020. https://doi.org/10.1134/S001679322008023X
  16. URL CME, hhttps://cdaw.gsfc.nasa.gov/CME_list
  17. URL Data GLE, hhttps://gle.oulu.fi
  18. URL IZMIRAN, hhttps://cr0.izmiran.ru
  19. URL Flares, hhttps://www.solarmonitor.org/
  20. URL GOES, hhttps://www.goes.noaa.gov/
  21. URL NMDB, hhttps://www.nmdb.eu/
  22. URL SEP, hhttps://umbra.nascom.nasa.gov/SEP/

Supplementary files

Supplementary Files
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2. Fig. 1. Relative intensity of primary protons with rigidities 2 (dashed line), 4 (solid thin line) and 6 GV (dashed line), as well as the relative intensity of secondary neutrons recorded by the NM at station. South Pole (solid thick line).

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3. Fig. 2. Spatial distribution of CR with a rigidity of 2 GV in the solar-ecliptic geocentric coordinate system at individual moments in time of GLE development: (a) before the event (01:30 UT), (b) maximum increase in CR intensity (02:00 UT) , (c) — after the event (02:50 UT).

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4. Fig. 3. Differential hardness spectra of primary protons, calculated from 5-minute data. The solid line is the calculated spectrum at the time of GLE (01:50 UT), the dashed line is the calculated spectrum before GLE (00:00 UT). Triangles mark observed GOES-10 data (for rigidities below 1 GV) and ground-based CR observations (for rigidities above 1 GV) at the time of GLE.

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5. Fig. 4. Differential hardness spectra of particles accelerated on the Sun at individual moments of GLE64: before the event (01:30 UT, solid line), at maximum CR intensity (02:00 UT, dashed line), after the event (02:50 UT, dotted line ).

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