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

Hinode/XRT reveals three eruptive features EF1, EF2, and

EF3EF1

EF2

EF3

Eruptions caused shocks and bursts

• Acceleration peaks occurred 2 min before 17 GHz peaks

Shock1 Shock2

EUV traces of two shock waves

EUV, LASCO, type II shock traces correspond to the shocks produced by two eruptions before the bursts

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.

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.

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).

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

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.

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.

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

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.

Our thanksOur thanks

For your attentionFor your attentionTo organizers of the meetingTo organizers of the meeting

To Nobeyama SRO colleagues To Nobeyama SRO colleagues