Kobayashi, Ken

Kobelski, Adam

Rachmeler, Laurel

Savage, Sabrina

Seaton, Daniel B.

West, Matthew J.

Winebarger, Amy

NASA Technical Reports Server

Observa(onal	Signatures	of	Magne(c	
Reconnec(on	in	the	Extended	Corona	
SabriNA	SAvage,	
Ma>hew	J.	West,	Daniel	B.	Seaton,	Adam	Kobelski	
Sabrina.Savage@nasa.gov	 *Considerable	contribu(ons	from	K.	Reeves	&	D.	McKenzie	
…..	and	First	Results	from	the	Hi-C	II	Sounding	Rocket	
Amy	Winebarger,	Ken	Kobayashi,	Laurel	Rachmeler	
https://ntrs.nasa.gov/search.jsp?R=20160012711 2019-08-29T17:22:33+00:00Z
Supra-Arcade	Downﬂows		
(SADs)	Observa(ons	
Fig	1:		McKenzie	&	Savage	2009	 Fig	2:		Savage	et	al.	2011		 Fig	3:		Savage	et	al.	2012	
Fig	1		
Fig	2		
Fig	3	
Fig	4		
2011	Oct	22,	SDO/AIA	
2011	May	9,	SDO/AIA	
Fig	5		
	
-  Teardrop-shaped	voids	observed	
to	travel	sunward	through	the	
bright,	hot	fan	extending	
outward	along	the	spine	of	
developing	post-ﬂare	arcades.	
-  Observed	with	high-temperature	
instrumenta(on	(EUV,	X-ray)	&	
white-light	coronagraph	(density)	
-  LONG	DURATION	EVENTS	
1999	Jan	20,	Yohkoh/SXT	
2002	Apr	21,	TRACE	
2010	Nov	4,	SOHO/LASCO	
Sadpoles,	not	tadpoles	
Supra-Arcade	Downﬂowing	Loops	
(SADLs)	Observa(ons	
Fig	1:		Savage	&	McKenzie	2011		
Fig	1		 2003	Nov	4,	TRACE	 2010	Nov	3,	SDO/AIA	
2000	Jan	1,	LASCO	
Fig	5	
Supra-Arcade	Downﬂowing	Loops	
(SADLs)	Observa(ons	
Fig	1:		Savage	&	McKenzie	2011		 Fig	2:		Savage	et	al.	2010		
Fig	1		
Fig	2	
2003	Nov	4,	TRACE	
2008	Apr	9,	Hinode/XRT	
Behind	the	limb	
Supra-Arcade	Downﬂowing	Loops	
(SADLs)	Observa(ons	
Fig	1:		Savage	&	McKenzie	2011		 Fig	2:		Savage	et	al.	2010		 Fig	3:		Savage	et	al.	2012		
Fig	1		
Fig	2	
Fig	3	
2003	Nov	4,	TRACE	
2008	Apr	9,	Hinode/XRT	
2010	Nov	3,	SDO/AIA	
Diﬀerent	from	Plasmoid	Observa(ons	
Fig	1:		Savage	et	al.	2010	
Fig	3		
Fig	4		
Fig	2		
Fig	3:		Takasao	et	al.	2012	 Fig	4:		Lin	et	al.	2004	Fig	2:		Ko	et	al.	2003	
Fig	1		
-  Coherent	‘bubble’	of	emi ng	plasma	held	
together	by	magne(c	ﬁelds.		
-  Observed	with	broadband-temperature	
instrumenta(on	(EUV,	X-ray,	Hard	X-ray)	&	
white-light	coronagraph	(density)	
Ø  Magne4c	Islands	
Diﬀerent	from	Plasmoid	Observa(ons	
Fig	1,	2:		Daughton	et	al.	2012	 Fig	3:		Nishizuka	et	al.	2013	
Fig	1	
Fig	2	
Fig	3	
-  Thin	ﬂux	tubes	
created	during	the	
reconnec(on	process	
across	the	current	
sheet.	
-  Plasmoids	a	3-D	
product	of	
reconnec(on	
concurrent	to	single	
loop	crea(on.	
SADs	+	SADLs	
-  Hot	AIA	channels.	(2-10	MK)	
-  Diﬀerenced	
-  Reverse-scaled		
SADs	+	SADLs	
Fig	1:		Savage	et	al.	2012			
Fig	1		 -  SADs	appear	to	be	voids	created	by	
loops	(SADLs)		shrinking	through	the	
fan	plasma.		
SADs	+	SADLs	
Fig	1,	2:		Savage	et	al.	2012			
Fig	1		
Fig	2		
-  SADs	appear	to	be	voids	created	by	
loops	(SADLs)		shrinking	through	the	
fan	plasma.		
Supra-Arcade	Downﬂowing	Loops	
(SADLs)	Observa(ons	
2012	Jan	27,	SDO/AIA	
Par(cle	Accelera(on	&	Hea(ng	
Fig	1:		Asai	et	al.	2004	(Khan;	Liu)	
Fig	1		
RHESSI	+	TRACE	
    
 
0
100
200
300
Di
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nc
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(a
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c)
Di
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(a
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AIA 94 cut 4
Flux Rope Eruption
17:00 18:00 19:00 20:00
 
0
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300
Di
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nc
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(a
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Di
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   18:45 19:00
Start Time (03-Mar-12 17:50:00)
50
100
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Di
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(a
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Di
sta
nc
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(a
rc
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AIA 94 cut 3
RHESSI 6-10 keV
VLA 1189 1317 1445
   18:45 19:00
 
 
 
 
  
AIA 131 cut 3
RHESSI 6-10 keV
VLA 1189 1317 1445
18:00 18:15 18:30 18:45 19:00
 
50
100
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Di
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(a
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Di
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(a
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Downflows
18:00 18:15 18:30 18:45 19:00
 
50
100
150
  Downflows
VLA	+	AIA	+	RHESSI	
Savage	–	2010	Nov	3	ﬂare	
Fig	3:		Chen	et	al.	2014;	2015	
Fig	2		
Fig	3		
RHESSI	+	AIA	
Diagram	Models	
Fig	1	 Fig		2	
Fig	3		
Fig	1,	2:		Savage	et	al.	2012	 Fig	3:		Ohyama	&	Shibata	2008	
3D	is	Pivotal	
Fig	1	
Fig		2	
Fig	3		
Fig	1,	2:		Savage	et	al.	2012	 Fig	3:		Ohyama	&	Shibata	2008	
Guidoni	&	Longcope	2010	
Fig	1:		Savage	et	al.	2012	
Fig	1	
-  Basic	reconnec(on	scenario,	post	
ini(al	ﬂux	rope	forma(on	and	
release.	
-  General	organiza(on	of	the	magne(c	
ﬁeld	of	the	various	components	
(SADs,	SADLs,	plasmoids).		
-  Field	lines	reconnect	across	the	
current	sheet	to	form	ouplowing	ﬂux	
tubes	while	plasmoids	form	along	the	
current	sheet.		
-  SADs	are	formed	as	the	ﬂux	tubes	
(SADLs)	retract	through	hot	plasma	in	
the	fan	(otherwise,	only	SADLs	are	
observed).		
Fig	1:		Savage	et	al.	2012	
Strong	poten(al	analogy	with		
magnetotail	substorms	
Dipolarization Front/
Bursty Bulk Flow
BBF Braking Region
South Pole** 
(ionosphere)
North Pole** 
(ionosphere)
Magnetotail 
current sheet
**Pole width exaggerated 
Pre-substorm Field
Line Geometry
Wakes 
Behind Dipolarization 
Fronts
To Sun
Fig	1	 Fig	2	
Fig	2:		Courtesy	of	A.	Kobelski,	Reeves	et	al.	2008	
Using	THEMIS	for	comparison	to	in	situ	data	
Courtesy	of	Adam	Kobelski	and	David	Malaspina	
Substan(al	density	drop	following	the	dipolariza(on	event!	
Model	Constraints	
Fig	1:		Savage,	McKenzie,	&	Reeves	2012	
OBSERVED	TEMPERATURE	AND	DENSITY	ALWAYS	LOWER	THAN	FAN	
Fig	1	
Fig	2:		Hanneman	&	Reeves	2014	
Fig	2	
Model	Simula(ons	
a)	
Pressure	pulse	+	MHD	wave		
	
(T	>>	fan)	
c)	
Peristal(c	pumping	
							
(T	~<		fan)	
b)	
Reconnec(on	ouplows		
	
(T	~<	fan)	
	
Too	hot	with	respect	
to	the	surroundings	
Fig	1:		Cecere	et	al	2012	
Incorrect	geometry	with	
respect	to	observa(ons	
Fig	3:		Sco>	et	al	2013	Fig	2:		Cassak	et	al	2013	
Incomplete,	feasible;	
Diﬃcult	to	match	to		
observa(ons	
Fig	1:		Guo	et	al	2014	
Rayleigh-Taylor	Instabili(es	behind	retrac(ng	ﬂux	tubes	(T	>	fan)	
Too	hot	with	respect	to	the	surroundings	 BUT	 Best	match	to	observa(ons	to	date	(3D!)	
although	early	in	development	
Model	Simula(ons	
SADs	in	the	Extended	Corona	
Fig	1	
Fig	1:		Sheeley,	Warren,	&	Wang	2007	
Fig	2	
Fig	2:		Sheeley	&	Wang	2007	
SADs	in	the	Extended	Corona…	
“Giant	Arches”	Flare	–	2014	Oct	14	
Fig	1:		West	&	Seaton	2015			
Fig	1	
PROBA-2/SWAP	–	174	Å		
~1.45	R¤	
SADs	in	the	lower	corona	are	typically	observed	
well	azer	reconnec(on	has	occurred.	
	
In	the	extended	corona,	we	are	be>er	able	to	
observe	the	migra(ng	reconnec(on	sites.	
	
Coronagraphs	allow	us	to	see	reconnec(on	
develop	behind	the	CME	while	looking	directly	
at	the	density.	
Go	see	MaBhew	West’s	talk	Friday	@	11:45	
SADs	in	the	Extended	Corona…	
PROBA-2/SWAP	GI	
LASCO	C2	
	PROBA-2/SWAP	
	 	AIA	131	Å	
	
A:		Fla>ened	from	a	year’s	
						worth	of	data	
							
						Cleaned	(cosmic	
						rays,	background	
						stars,	planets)	
							
						A>enuated	disk	
	
B:		Smooth-Diﬀerenced	
	
-	Scaled	
B	A	
SADs	in	the	Extended	Corona…	
LASCO	C2	
	PROBA-2/SWAP	
	 	AIA	131	Å	
	
C:		Run-Mean-Diﬀerenced	
	
D:		Smooth-Diﬀerenced	
							
						Extracted	
	
-	Scaled	
C	 D	
SADs	in	the	Extended	Corona…	
40	Flows	Tracked	
Median	~	-82	km/s	
Velocity	[km/s]	
#	
of
	o
cc
ur
re
nc
es
	
SADs	in	the	Extended	Corona…	
-2000 0 2000 4000 6000 8000
Elapsed Flow Time [min]
1000
2000
3000
4000
5000
6000
He
igh
t [
M
m]
All Flows
He
ig
ht
	[M
m
]	
Elapsed	EVENT	Time	[min]	
0 100 200 300 400
Elapsed Flow Time [min]
1000
2000
3000
4000
5000
He
igh
t [
M
m]
All Flows
He
ig
ht
	[M
m
]	
Elapsed	FLOW	Time	[min]	
Individual	ﬂow	proﬁle	
Trend	in	ini(al	heights	
SADs	in	the	Extended	Corona…	
TBD	
1.  Correlate	
ﬂows	directly	
to	lightcurve	
as	done	for	
2010	Nov	3rd	
event	
2.  Spa4ally	and	
temporally	
correlate	
RHESSI	and	
Hinode/XRT	
X-ray	
contours	with	
ou^lows.	
Summary	&	Forward	Work	
•  Con(nua(on	of	shrinking	loops	imparts	energy	into	the	current	sheet	
long	azer	the	ﬂare.		Clearly.	
–  But	for	an	en(re	week??	
–  Does	this	happen	all	of	the	(me?	
–  How	did	this	one	grow	so	large? 		
•  Density	stra(ﬁca(on?		Ac(ve	region	interac(ons?	
•  Reconnec(on	is	fast	and	patchy.	
•  Add	Hinode/XRT	and	RHESSI	data	(started).	
•  Do	features	track	between	ﬁelds	of	view	both	ways?	
–  Ini(al	work	begun.		(Some	even	in	LASCO	C3.)	
•  Need	for	instrumenta(on	to	ﬁll	the	gap	in		
					observing	the	transi(on	corona	
–  Important	to	be	in	single	wavelength	
–  Possibly	coming	to	an	Interna(onal	Space	Sta(on	
						near	you….	

Hi-C	2	Status	
A B Cbackshell
connector
short
•  Beau(ful	ﬂight,	even	azer	a	week	of	de ay	
•  Science	images	not	captured	due	to	the	
camera	shu>er	not	opening	
•  Loads	of	calibra(on	images	from	the	new	
MSFC	camera	design	
•  Achieved	low	noise	requirements	
•  Anxious	to	reﬂy	
13	e-	rms	
7	e-	rms	 7	e-	rms	
8	e-	rms	


Observational Signatures of Magnetic Reconnection in the Extended Corona and First Results from the Hi-C II Sounding Rocket

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