TRACE+RHESSI;,courtesy, S.,Krucker,,SSL,Berkeley,
• Late,parScle,acceleraSon,associated,with,the, development,of,flare,ribbons,and,the,
formaSon,of,an,EUV,arcade,
Klein,,Masson,et,al.,2014,AA,572,,A4,
Freq (MHz)
ARTEMIS IV DYNAMIC & DIFFERENTIAL SPECTRUM: 2005−01−20
50
100 150 200 300 400 500600
Freq (MHz)
06:55 07:00 07:05
50
100 150 200 300 400 500600
• Narrow,bandwidth,,
slow,frequency, drii:,like,a,type,II, burst,
• But:,none,of,the, typical,type,II,fine, structures,(F/H,, band,spliÜng,, herringbone, bursts)
,
Mann,et,al.,,2003,A&A,400,, 329,
• Instead:,spectral, features,typical,of, type,IV,bursts, (conSnuum,,
electrons,confined, in,coronal,
magneSc, structures),
• Why,does,this,
burst,drii,towards, lower,
frequencies,?,
The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,
The,second,release,of,GeV%protons,–shock,vs,coronal,current,sheets ,
Klein,,Masson,et,al.,2014,AA,572,,A4,
space,
Nançay,
23,
• No,imaging,observaSons,of,the, 2005,Jan,20,type,IV,burst.,
IllustraSon,with,a,different,event:, 2012,Mar,04,
• Dynamic,spectrum:,
– Succession,of,two,conSnua,at,dm%m%λ, – The,first,is,broadband,without,
frequency,drii,in,the,1000%300,MHz, range,,then,develops,a,drii,to,lower, frequencies,(200%40,MHz;,similar,to, 2005,Jan,20),
– The,second,remains,confined,to,ν>100, MHz,,more,complex,spectral,structure,
1, 2,
The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,
The,second,release,of,GeV%protons,–shock,vs,coronal,current,sheets ,
Nançay,RH,
150,MHz,
24,
• No,imaging,observaSons,of,the, 2005,Jan,20,type,IV,burst;,
illustraSon,with,a,different,event:, 2012,Mar,04,
• Dynamic,spectrum:,
– Succession,of,two,conSnua,at,dm%m%λ, – The,first,is,broadband,without,
frequency,drii,in,the,1000%300,MHz, range,,then,develops,a,drii,to,lower, frequencies,(200%40,MHz;,similar,to, 2005,Jan,20),
– The,second,remains,confined,to,ν>100, MHz,,more,complex,spectral,structure,
• NRH,observaSons,at,150,MHz:,
– the,first,type,IV,conSnuum,has,a,source, with,systemaSc,outward,moSon,
(moving,type,IV,burst),
– the,2nd,conSnuum,comes,from,
~staSonary,sources,underneath,,,
The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,
The,second,release,of,GeV%protons,–shock,vs,coronal,current,sheets ,
• Well%known,scenario,from,earlier,observaSons:, parScle,(here:,electron),acceleraSon,in,the,current, sheet,in,the,aiermath,of,a,CME,,
– Review,of,early,work:,,
• Stewart,1985,,in,McLean,&,Labrum,,Solar,Radiophysics,
– InterpretaSon,of,spectrographic,observaSons:,
• Kliem,et,al.,2000,AA,360,,715,
• Aurass,et,al.,2009,AA,506,,901,(+UVCS),
– NRH,observaSons:,
• Klein,&,Mouradian,2002,AA,381,,683,
• Vrsnak,et,al.,2003,SP,214,,325,
• Pick,et,al.,2005,ApJ,625,,1019,
• Démoulin,et,al.,2012,ApJ,750,,147,
25,
The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,
The,second,release,of,GeV%protons,–,shock,vs,coronal,current,sheets ,
• SEP,acceleraSon,in,the,post%CME,current,sheet:,
– Early,idea,(Carmichael,,1964).,Models,by,Litvinenko,&,Somov, (1995,SP,158,,317),,Akimov,et,al.,(1996,SP,166,,107),,Ryan, (2000,SSR,93,,581),,Litvinenko,(2006,AA,452,,1069),,
Heerikhuisen,et,al.,(2002,ApJ,566,,512),,Chupp,&,Ryan,(2009,, Res,AA,9,,11),,Podgorny,et,al.,(2010,,JASTP,72,,988),,
– QuanStaSve,invesSgaSons,so,far,based,on,MHD,models,+, test,parScles,(cf.,P.,Browning),
Freq (MHz)
ARTEMIS IV DYNAMIC & DIFFERENTIAL SPECTRUM: 2005−01−20
50
100 150 200 300 400 500600
Freq (MHz)
06:55 07:00 07:05
50
100 150 200 300 400 500600
• Type,III,bursts,<,14,MHz:,evidence,for, access,of,electrons,to,IP,space,
- no,direct,connecSon,to,the,type,IV, conSnuum;,
- spectral,fine,structure,80%20,MHz:, evidence,of,reconnecSon,between,the, expanding,magneSc,structure,and,open, neighbouring,fields,(Masson,et,al.,2013,,ApJ,, 771,,82),?,
The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,
ParScle,escape,to,the,IP,space ,
The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,
Summary ,
• The,GLE,shows,a,remarkable,correspondence,of,two,SEP,releases,with,radio, and,UV,emission.,
• Provided,these,similariSes,can,be,ascribed,to,a,common,physical,origin,of,the, radiaSng,electrons,and,the,escaping,relaSvisSc,protons,,these,observaSons, suggest,an,important,role,of,magneSc,reconnecSon,in,the,process,of,
relaSvisSc,proton,acceleraSon.,
• Although,a,fast,CME,existed,and,most,likely,drove,a,strong,shock,since,the,low, corona,,we,found,no,concurrent,Sming,of,type,II,emission,with,either,of,the, two,relaSvisSc,proton,releases.,
• Comparison,with,two,other,GLEs:,
27,
28,
• Two,intervals,of,solar,radio,emission,,the, second,more,pronounced,at,lower,radio, frequencies,(similar,to,2005,Jan,20),
• RelaSvisSc,protons,at,1,AU,(GLE;,different, from,2005,Jan,20):,
– a,single,pulse,of,relaSvisSc,protons,,(see,Moraal,
&,Caballero%Lopez,2014,,ApJ,790,,154),
– substanSal,delay,of,the,GLE,onset,wrt,the,first, radiaSve,signatures,of,parScle,acceleraSon,in, the,corona:,~30%40,min,(~5,min,on,2005,Jan, 20),
• Parent,acSvity,≥,W,90°,
Other,relaSvisSc,solar,parScle,events,(GLEs):,29,Sep,1989,
Radio,emission,and,relaSvisSc,proton,release ,
Klein,et,al.,1999,,AA,348,,271,
29,
• What,is,the,Sming,relaSonship,between,the, electrons,(parScles),at,the,Sun,and,the,
protons,at,1,AU,?,
RelaSvisSc,solar,parScle,events,(GLEs):,29,Sep,1989,
Radio,emission,and,relaSvisSc,proton,release ,
Klein,et,al.,1999,,AA,348,,271,
• A,simple,model:,radio,emission, as,the,injecSon,funcSon,,free, streaming,to,1,AU,,L=1.3,AU,
• Result:,
– no,contribuSon,of,impulsive,phase,acceleraSon,, – relaSvisSc,p,release,with,the,late,phase,of,
coronal,acceleraSon,(reconnecSon,in,the,post%
CME,current,sheet),
30,
• Similar,to,1989,Sep,29:,
– two,intervals,of,solar,radio,emission,,the, second,more,pronounced,at,lower,radio, frequencies,(similar,to,2005,Jan,20;,driiing, conSnuum),
– a,single,pulse,of,relaSvisSc,protons,(see,Moraal,&, McCracken,2012,,SpSR,171,,85),,,
– substanSal,delay,of,the,GLE,onset,wrt,the,first, radiaSve,signatures,of,parScle,acceleraSon,in, the,corona:,~20,min,(~5,min,on,2005,Jan,20),
• Parent,acSvity,W,07°,
• Again,a,beFer,Sming,relaSonship,with,the, late,radio,emission,(type,IV,burst),
RelaSvisSc,solar,parScle,events,(GLEs):,14,Jul,2000,
Radio,emission,and,relaSvisSc,proton,release ,
Klein,et,al.,2001,,AA,373,1073,
31,
• Similar,to,1989,Sep,29:,
– two,intervals,of,solar,radio,emission,,the, second,more,pronounced,at,lower,radio, frequencies,(similar,to,2005,Jan,20;,driiing, conSnuum),
– a,single,pulse,of,relaSvisSc,protons,(see,Moraal,&, McCracken,2012,,SpSR,171,,85),
– substanSal,delay,of,the,GLE,onset,wrt,the,first, radiaSve,signatures,of,parScle,acceleraSon,in, the,corona:,~23,min,(~5,min,on,2005,Jan,20),
• Parent,acSvity,W,07°,
• Again,a,beFer,Sming,relaSonship,with,the, late,radio,emission,(type,IV,burst),
• Moving,source,=,evidence,of,parScle, acceleraSon,in,the,post%erupSve,current, sheet,
RelaSvisSc,solar,parScle,events,(GLEs):,14,Jul,2000,
Radio,emission,and,relaSvisSc,proton,release ,
Klein,et,al.,2001,,AA,373,1073,
On,the,origin,of,relaSvisSc,solar,parScle,events,
Summary ,
• RelaSvisSc,SEP,events,(GLEs),display,a,temporal,structure,with,similariSes,to, radiaSve,signatures,of,parScle,(electron),acceleraSon,in,the,corona.,
• The,study,of,3,GLEs,suggests,a,close,relaSon,between,the,release,of,relaSvisSc, protons,and,EM,emissions,of,accelerated,parScles,(electron%biased,!),at,the, Sun.,
• Results,suggest,the,importance,(or,even,predominance),of,processes,related,to, magneSc,reconnecSon,to,understand,the,origin,of,the,highest,SEP%energies.,
• CMEs,are,essenSal,for,the,enSre,process,,but,apparently,due,to,the,
reconnecSon,of,,or,turbulence,in,,the,magneScally,stressed,corona,in,their, aiermath,rather,than,due,to,their,shock,waves.,
• New,opportuniSes,for,comparaSve,Sming,studies,with,Solar#Orbiter,close,to, the,Sun,!,
32,