AN INTERPRETATION OF GLE71 CONCURRENT CME-DRIVEN SHOCK WAVE

Journal Article · Fri Aug 01 04:00:00 EDT 2014 · Astrophysical Journal, Supplement Series

DOI:https://doi.org/10.1088/0067-0049/213/2/24· OSTI ID:22340188

Firoz, Kazi A.; Rodríguez-Pacheco, J. ^[1]; Zhang, Q. M.; Gan, W. Q.; Li, Y. P. ^[2]; Moon, Y. -J. ^[3]; Kudela, K. ^[4]; Park, Y. -D. ^[5]

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1. Space Research Group, Universidad de Alcalá, E-28871 Alcalá de Henares (Spain)
2. Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210008 Nanjing (China)
3. School of Space Science, Kyung-Hee University, 446-701 Yongin-Si, Gyeonggi-do (Korea, Republic of)
4. Institute of Experimental Physics, Slovak Academy of Sciences, Watsonova 47, 04001 Kosice (Slovakia)
5. Korea Astronomy and Space Science Institute, Daejeon 305-348 (Korea, Republic of)

Particle accelerations in solar flares and CME-driven shocks can sometimes result in very high-energy particle events (≥1 GeV) that are known as ground level enhancements (GLEs). Recent studies on the first GLE event (GLE71 2012 May 17 01:50 UT) of solar cycle 24 suggested that CME-driven shock played a leading role in causing the event. To verify this claim, we have made an effort to interpret the GLE71 concurrent shock wave. For this, we have deduced the possible speed and height of the shock wave in terms of the frequency (MHz) of the solar radio type II burst and its drift rate (MHz min{sup –1}), and studied the temporal evolution of the particle intensity profiles at different heights of the solar corona. For a better perception of the particle acceleration in the shock, we have studied the solar radio type II burst with concurrent solar radio and electron fluxes. When the particle intensity profiles are necessarily shifted in time at ∼1 AU, it is found that the growth phases of the electron and cosmic ray intensity fluxes are strongly correlated (>0.91; ≥0.87) with the frequency drift rate of the type II burst, which is also consistent with the intensive particle accelerations at upper coronal heights (∼≥0.80 R {sub S} < 1.10 R {sub S}). Thus, we conclude that the CME-driven shock was possibly capable of producing the high-energy particle event. However, since the peaks of some flare components are found to be strongly associated with the fundamental phase of the type II burst, the preceding flare is supposed to contribute to the shock acceleration process.

• OSTI ID: 22340188
• Journal Information: Astrophysical Journal, Supplement Series, Journal Name: Astrophysical Journal, Supplement Series Journal Issue: 2 Vol. 213; ISSN 0067-0049; ISSN APJSA2
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ACCELERATION
COSMIC RADIATION
ELECTRONS
GEV RANGE
GROUND LEVEL
MHZ RANGE
SHOCK WAVES
SOLAR CORONA
SOLAR CYCLE
SOLAR FLARES
VELOCITY