On#the#Origin#of## Relafivisfic#Solar#Parficle#Events,

Karl%Ludwig,Klein, ludwig.klein@obspm.fr,!

On#the#Origin#of##

Rela/vis/c#Solar#Par/cle#Events

^,

(F%92195,Meudon),

Univ,P&M,Curie,,Paris,Diderot,

Collaborators:,G.,TroFet,,S.,Masson,(Meudon),,,

C.,Bouratzis,,A.,Hillaris,,P.,Preka%Papadema,(Athens),,, V.,Grechnev,(Irkutsk),

•  Solar,energeSc,parScle,events,

•  Scenarios,of,acceleraSon,

•  Timing,relaSonships,between,relaSvisSc,protons,at,1,AU,and, EM,emissions,at,the,Sun,

–  a,case,study:,2005,Jan,20,

–  two,further,GLEs:,1989,Sep,29,,2000,Jul,14

,

•  Conclusions,

On,the,Origin,of,RelaSvisSc,Solar,ParScle,Events,

Outline ,

2,

flare,

p>10,MeV,

p>450,MeV, ^3,days,

www.nmdb.eu,

©,SoHO,ESA/NASA,

SXR,

cdaw.gsfc.nasa.gov/CME_list/,

Solar,energeSc,parScle,(SEP),events,

An,illustraSon ,

3,

Solar,energeSc,parScle,events,

Scenarios,of,acceleraSon,

•  “Flare,acceleraSon”,:,,

–  reconnecSng,current,sheet,,induced,E,, waves,,possibly,reconnecSon,shock,, –  acSve,region,,mainly,low,corona,

–  parScles,revealed,by,radiaSve,signatures, (gamma,,HXR,,radio),,evidence,for,e(>10, MeV),,p(>300,MeV),

•  “CME,acceleraSon”,:,,

-  fast,CME,drives,shock,wave,

-  parScles,scaFered,between,shock,and,upstream, turbulence,(“diffusive,shock,acceleraSon”),or,drii, along,shock,front,(“shock,drii,acceleraSon”),

-  evidence,in,situ,(up,to,which,energy,?),

-  In,addiSon:,magneSc,reconnecSon,in,the,post%CME, current,sheet,

Aier,K.%L.,Klein.,,Solar#Orbiter,Workshop,,Athens,,ESA%SP,

5,

The,origin,of,solar,energeSc,parScle,(SEP),events,

AcceleraSon,scenarios ,

•  But:,

–  Do,conclusions,drawn,from,observaSons,~1,MeV/nuc,apply,at,higher, energies,?,

•  Since,the,1990s:,disSncSon,of,2,classes,of,events,,impulsive,(small;, frequent;,“flare%related”),and,gradual,events,(large;,rare;,“CME%shock, related”).,,

•  MoSvaSon:, _C.M.

S.,Cohen,,2003,ICRC,,Rapporteur,paper,

‘impulsive’,

‘gradual’, –  elemental,

abundances,,ionic, charge,states,∼,1, MeV/nuc;,

–  the,presumed, plausibility,of, coronal,shocks,as, parScle,accelerators, (see,Reames,1999, Spa,Sci,Rev,90,,413),,

The,origin,of,solar,energeSc,parScle,(SEP),events,

Two,classes,of,SEP,events,? ,

6,

–  Energy,dependence,of,the,correlaSons:, dominant,CME,speed,(<,20,MeV),%>, dominant,SXR,flux,(>,20,MeV;,

Dierckxens,et,al.,2015,,SP,online#first),

•  Large,SEP,events,are,associated,with,both,flares,and,fast,CMEs,

•  StaSsScs:,,

–  Broad,(Pearson),correlaSons,of,SEP,peak,intensiSes,with,many,parameters,of, erupSve,acSvity,(CME,speed,,SXR,peak,flux,,SXR,fluence,,microwave,fluence;, Kahler,1982,,2001,,Gopalswamy,et,al.,2003,,2004,,Belov,et,al.,2007,,Cliver,&, Dietrich,2013,,Cliver,et,al.,2014,,Miteva,et,al.,2013),

–  ParSal,correlaSon,analysis:,significant,dependence,,of,p(15%40,MeV),intensity, on,both,CME,speed,and,SXR,fluence,(TroFet,et,al.,2015),

,

The,origin,of,solar,energeSc,parScle,(SEP),events,

Two,classes,of,SEP,events,%,staSsScal,evidence,? ,

7,

•  Conclusion:,,

–  Both,CME,shocks,and,flares,contribute, to,large,SEP,events,

–  The,relaSve,contribuSon,depends,on,the, parScle,energy,

Dierckxens,et,al.,2015,,Solar,Phys.,

Event-integrated energy spectra during two large SEP events (ACE & Wind; Tylka et al 2005 ApJ 625, 474; Rouillard et al. 2012 ApJ 752, 44)

•  Elemental,abundances,in,SEP, events,seen,at,different,energies,

•  Fe/O,raSo:,marked,increase,with, increasing,energy,>1,MeV/nuc.,

•  InterpretaSon,

–  Seed,populaSons,accelerated,by, CME,shock,may,be,enriched,by, flares,(“flare,suprathermals”), –  ContribuSon,of,flare%accelerated,

parScles,at,high,energies,?,

The,origin,of,solar,energeSc,parScle,(SEP),events,

Two,classes,of,SEP,events,–,the,abundance,argument ,

8,

Event-integrated Fe charge state during large SEP events (STEREO, ACE, SoHO; compiled by Klecker et al 2007 SpSR 130, 273)

•  Ionic,charge,states,in,SEP,events, seen,at,different,energies:,

–  Low,charge,states,at,low,energies, (blue;,≤,1,MeV/nuc),,

–  Higher,charge,states,at,higher, energies,(red;,>28,MeV/nuc),,

–  Overall:,broad,scaFer,,up,to,typical,

“impulsive,SEP”,values,(Q_FE=20),at, the,higher,energies,

,

•  InterpretaSon,

–  Seed,populaSons,accelerated,by, CME,shock,may,be,enriched,by, flares,(“flare,suprathermals”), –  ContribuSon,of,flare%accelerated,

parScles,at,high,energies,?,

The,origin,of,solar,energeSc,parScle,(SEP),events,

Two,classes,of,SEP,events,–,the,charge,state,argument ,

Typical,«,impulsive,»,

Typical,«,gradual,»,

9,

•  CME%shock,acceleraSon,,

–  convincingly,demonstrated,for,MeV,–,10s,of,MeV,protons,and,ions,

–  widely,considered,as,the,principal,accelerator,of,ions,and,protons,in,large,SEP, events,(generalisaSon,of,observaSonal,evidence,at,lower,energies).,

•  DifficulSes,to,reconcile,the,simple,shock%acceleraSon,picture,of,the,1990s, with,more,recent,in,situ,measurements,are,solved,(?),by,assumpSons:,

–  flare,suprathermals,as,seed,populaSon,for,shock,acceleraSon,

–  rigidity%dependent,parScle,transport,in,the,turbulent,IP,magneSc,field.,

•  Plausible,assumpSons,,but,,

–  liFle/no,independent,support,,especially,at,energies,>>,10,MeV,

–  coronal,shocks,(type,II,radio,bursts),are,not,necessarily,efficient,proton, accelerators,

–  no,jusSficaSon,why,flare%accelerated,parScles,do,not,contribute,to,major,SEP, events.,

10,

The,origin,of,solar,energeSc,parScle,(SEP),events,

Two,classes,of,SEP,events,–,status,of,the,discussion,2015 ,

Solar,parScle,acceleraSon,to, relaSvisSc,energies:,GLEs,

A,case,study,using,radiaSve,

diagnosScs,and,in,situ,measurements,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

GeV%protons,at,Earth:,neutron,monitor,observaSons ,

•  A,large,solar,flare,and,fast,CME,on, 20,Jan,2005,,where,relaSvisSc,

protons,were,observed,at,the,Earth, ,

•  Key,observaSon:,the,relaSvisSc, proton,profile,has,two,peaks,(two, successive,parScle,releases,at,the, Sun),

•  Double%peak,structure,seems,to,be, characterisSc,of,well%connected, strong,GLEs,(Moraal,&,McCracken,2012, SpSR,171,,85;,McCracken,et,al.,2012,ApJ,761,, 101):,

-  iniSal,anisotropic,pulse,,fast,rise, and,decay,

-  followed,by,less,anisotropic,pulse, seen,by,the,bulk,of,the,NMs,

Moraal,&,McCracken,2012,SpSR,171,,85,,

•  Double%peaked,structure,also,shown, in,the,intensity,Sme,histories,of,the, relaSvisSc,protons,(analysis,by,

BueSkofer,et,al.,,see,Masson,et,al.,2009,SP, 257,,305),

06:30 06:50 07:10 07:30 07:50

0.0 0.5 1.0 1.5 2.0

0 1 2-4 5 6

06:30 06:50 07:10 07:30 07:50

0.0 0.5 1.0 1.5 2.0

Proton intensity [rel. units]

Neutron monitor network (Time axis - travel 216 s)

2 GV

(e) 5 GV

•  Two,successive,proton,releases,,for,

-  both,pulses,show,protons, streaming,anS%sunward,

-  second,pulse,too,early,for,protons, reflected,by,a,barrier,beyond,1,AU,,

•  RelaSonship,with,parScle,

acceleraSon,signatures,at,the,Sun,?,

Moraal,&,McCracken,2012,SpSR,171,,85,,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

GeV%protons,at,Earth:,neutron,monitor,observaSons ,

Klein,,Masson,et,al.,2014,AA,572,,A4,

Soi,X%rays:,plasma,heaSng,in,the, flaring,acSve,region,to,several,10⁷,K, Microwaves,(ν>1,GHz),(or,hard,X%rays),as,tra%

cers,of,NT,e,in,the,low,corona,to,100s%1000s, of,keV,(gyrosynchrotron,radiaSon), Radio,(1,GHz%100,MHz):,NT,e,in,the,middle, corona,(≤,0.7,R_S,above,photosphere), Radio,(80,MHz%20,kHz,):,NT,e,between,the,high, corona,(≈1,R_S),and,the,Earth,(20,kHz);,most, prominent:,e,beams,travelling,from,Sun,to,Earth, Time,profiles,of,relaSvisSc,protons,at,1,AU,

(worldwide,neutron,monitor,network),

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

GeV%protons,at,Earth,,radio,and,X%ray,emission ,

Klein,,Masson,et,al.,2014,AA,572,,A4,

•  At,≥,dm%λ,waves:,emission,at,ν~ν_pe~√n_e^,

–  PropagaSng,exciter,in,a,quasi%staSc, atmosphere,or,expanding,loops,(CME):,

–  CharacterisSc,shapes,of,the,radio,burst,spectra:,

Type,IV,, (trapped,e),

trapped,e, e,beam, shock,,

Frequency,[MHz],

Time,(alStude),

II, III,

IV,

Type,III,, (e,beams),

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

Nature,of,the,dm%km%wave,emission ,

Type,II,, (shock,wave),?,

or,type,IV,, (trapped,e),?,

Klein,,Masson,et,al.,2014,AA,572,,A4,

•  Two,broad,intervals,of,electron,

(parScle),acceleraSon,also,evident,in, the,radio,signatures.,

•  Type,III,bursts,demonstrate,that, electrons,(parScles),escape,to,IP, space,during,both,intervals.,

•  Timing,relaSonship,between,the, relaSvisSc,protons,at,1,AU,and,the, radiaSve,signatures,(Sun%to%Earth),?,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

GeV%protons,at,Earth,,radio,and,X%ray,emission ,

Klein,,Masson,et,al.,2014,AA,572,,A4,

•  The,first,relaSvisSc,proton,pulse:, relaSvisSc,electrons,&,protons,in,the, solar,atmosphere,

•  Spectrum,hν>,60,MeV,(V.,Kurt,,B., Yushkov;,CORONAS/SONG):,photons, from,π%decay,

•  AcceleraSon,of,protons,to,>,300,MeV, during,the,impulsive,flare,phase,

(≥06:45),

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

The,first,release,of,GeV%protons:,acceleraSon,in,the,solar,atmosphere ,

Masson,et,al.,2009,SP,257,,305,

Klein,,Masson,et,al.,2014,AA,572,,A4,

•  The,first,relaSvisSc,proton,pulse:, protons,at,1,AU,vs,electron,escape, from,the,corona,(type,III),

type,III,(~14,MHz),

protons,(5,GV),

Shii,%216,s,

•  First,observaSonal,signature,of,electron, (parScle),release,to,IP,space,~06:45,

•  RelaSvisSc,protons,accelerated,with, those,emiÜng,π%decay,γs,can,escape,!,

•  Travel,path,to,Earth:,~1.5,AU.,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

The,first,release,of,GeV%protons:,escape,to,IP,space ,

•  RelaSvisSc,proton,acceleraSon,in, the,corona,during,the,impulsive, flare,phase,

•  MagneSc%reconnecSon,scenario, suggested,by,TRACE/RHESSI, movie,(courtesy,S.,Krucker),

•  Consistent,with,the,first,pulse,of, the,GLE,detected,at,Earth,(IP,

travel,1.5,AU:,longer,than,Parker,, but,consistent,with,disturbed, IMF;,Masson,et,al.,2012,AA,538,, A32)

,

19,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

The,first,release,of,GeV%protons:,scenario,of,acceleraSon ,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

The,second,release,of,GeV%protons ,

Klein,,Masson,et,al.,2014,AA,572,,A4,

The,relaSvisSc,solar,parScle,event,of,2005,Jan,20,

The,second,release,of,GeV%protons ,

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,2^nd,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,