The 2006-12-13 event included major flare, fast CME, strong shock, big SEP event and GLE70.
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Transcript of The 2006-12-13 event included major flare, fast CME, strong shock, big SEP event and GLE70.
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Eruptions, shock waves, and Eruptions, shock waves, and major flare in the 2006-12-13 major flare in the 2006-12-13
eventeventV. Grechnev, V.Kiselev, A.Uralov, N.Meshalkina
The 2006-12-13 event included major flare, fast CME, strong shock, big SEP event and GLE70.
We endeavor:– to clarify relations between eruptions, shock, and the flare – to shed light on two concepts of SEP origin: flare processes or bow shock driven by CME at 2-4 R.
Solar Physics with Radio Observations – Twenty Years of Nobeyama Radioheliograph and Beyond –
Dedicated to the memory of T. Kosugi
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Hinode/XRT reveals three eruptive features EF1, EF2, and
EF3EF1
EF2
EF3
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Eruptions caused shocks and bursts
• Acceleration peaks occurred 2 min before 17 GHz peaks
Shock1 Shock2
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EUV traces of two shock waves
EUV, LASCO, type II shock traces correspond to the shocks produced by two eruptions before the bursts
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Conclusions from Hinode/XRT & SOT, NoRH & NoRP, HiRAS,
LASCO data• Major flare lots of high-energy electrons
injected in strongest magnetic fields above sunspot umbrae.
• Shocks developed much earlier than assumed and could accelerate protons before the flare peak.
• Delayed CME-driven bow-shock hypothesis is not confirmed.
• Late particle release time does not support exceptional shock-acceleration of solar energetic particles.
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Relations between strong high-frequency radio bursts and big
proton eventsV.Grechnev, N.Meshalkina, I.Chertok
• Causes of well-known correlation between SEP events and strong high-frequency bursts are subject of debates.
• Irrespective of SEP origins, we analyze relations between ~100 NoRP bursts with Flux35 GHz > 1000 sfu in 1990–2012, on the one hand, and SEP events, on the other hand.
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Results: three groups of events
1. At least, 74% bursts with F35 GHz > 104 sfu bursts were associated with protons Jp100 > 1 pfu.
2. Three inconclusive big SEP events were associated with backside eruptions.
3. Four exceptions with 102 < F35 GHz < 103 sfu and large protons fluxes: – 2000-11-08, – 2001-12-26 (GLE63), – 2002-04-21, – 2012-05-17 (GLE71).
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Exceptions
General correspondence between most SEP events and fluxes at 35
GHz• Direct F35 GHz – SEP relation widespread
around Jp100 ~ (F35/5000)2
• Extreme bursts at 35 GHz indicate flaring abovesunspot umbrae
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Conclusions• Flares above sunspot umbrae favor big SEP
events. • Promptest alert of SEP events:
– Strong high-frequency bursts; – Flare ribbons crossing sunspot umbrae.
• Extreme bursts at 35 GHz indicate big SEP events with hard energy spectra.
• Big SEP enhancements associate with moderate microwave bursts need understanding.
• NoRP & NoRH observations highly important in further investigating into SEP problem.
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What multi-wave observations of microwave negative bursts tell us
about solar eruptions?V.Grechnev, I.Kuzmenko, A.Uralov, I.Chertok
• Cool plasmas of eruptive filaments can occult compact sources and quiet solar areas. Absorption can be observed as microwave ‘negative bursts’ and large depressions in He II 304 Å line.
• Two presented events show ‘anomalous’ eruptions with disintegration of eruptive filament and dispersal of its remnants as a cloud over a large solar surface.
• Possible scenario of anomalous eruption is proposed.
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Anomalous eruption on 2011-06-07 in SDO/AIA 304 Å images
• Suggests reconnection between filament’s internal magnetic fields and surrounding coronal magnetic fields
• NoRP: negative burst
06:11 06:37 06:54 07:41 08:11
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NoRP & NoRH observations have revealed
• Different kinds of negative bursts: – well-known post-burst decrease; – isolated negative bursts without preceding flare bursts.
• Negative bursts caused by occultation of – compact sources;– large quiet-Sun areas.
• Two scenarios of occultation by – steadily expanding filament; – remnants of a filament dispersed in an anomalous eruption.
• Anomalous eruptions and their expected properties.• Parameters of ejected plasma can be estimated from
multi-frequency records of negative bursts.• Ongoing observations with NoRP and NoRH
can shed further light on different scenarios and parameters of solar eruptions.
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Our thanksOur thanks
For your attentionFor your attentionTo organizers of the meetingTo organizers of the meeting
To Nobeyama SRO colleagues To Nobeyama SRO colleagues