Solar-B Science MeetingKyoto, Nov. 9, 2005 Quantifying Reconnection* Dana Longcope, Dave McKenzie Jonathan Cirtain, Jason Scott Montana State University.

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Presentation transcript:

Solar-B Science MeetingKyoto, Nov. 9, 2005 Quantifying Reconnection* Dana Longcope, Dave McKenzie Jonathan Cirtain, Jason Scott Montana State University * NASA grant NAG * NASA grant NAG

Solar-B Science MeetingKyoto, Nov. 9, 2005 Outline What happened in Aug. 2001What happened in Aug Cataloging interconnectionsCataloging interconnections Making a magnetic modelMaking a magnetic model Interp’ing data w.r.t. the modelInterp’ing data w.r.t. the model What does it tell us about reconnectionWhat does it tell us about reconnection

Solar-B Science MeetingKyoto, Nov. 9, 2005 Case study: AR 9574 PHOTOSPHERE :51 UT AR9570 AR9574 movie

Solar-B Science MeetingKyoto, Nov. 9, 2005 Case study: AR 9574 PHOTOSPHERE CORONA TRACE 171A (10 6 K Plasma) :51 UT movie

Solar-B Science MeetingKyoto, Nov. 9, 2005 Timeline of emergence 00:0012:0000:0012:00 Aug 10, 2001 Aug 11, :00 PHOTOSPHERE CORONA 7:34

Solar-B Science MeetingKyoto, Nov. 9, 2005 Why this is reconnection Emerged flux Reconnected flux Old flux Baum & Bratenahl1976

Solar-B Science MeetingKyoto, Nov. 9, 2005 Interconnecting loops: A catalog Synthetic slit TRACE 171 images: sec 7:00 Aug10 – 23:59 Aug11 BG subtracted

Solar-B Science MeetingKyoto, Nov. 9, 2005 Stack slit pixels… Time after 00:00 Aug10 11:00 Aug10 11:00

Solar-B Science MeetingKyoto, Nov. 9, 2005 Loops are bright features

Solar-B Science MeetingKyoto, Nov. 9, 2005 Lots of loops:~9:00  14:00 Gen’lbright’g 1 st loop: 12:36

Solar-B Science MeetingKyoto, Nov. 9, 2005 Finding the loops Identify peaks Identify peaks in slit-intensity in slit-intensity loop = hm loop = hm

Solar-B Science MeetingKyoto, Nov. 9, 2005 Finding the loops Identify peaks Identify peaks in slit-intensity in slit-intensity loop = hm loop = hm

Solar-B Science MeetingKyoto, Nov. 9, 2005 Finding the loops Show peaks vs. time Loop = row of peaks

Solar-B Science MeetingKyoto, Nov. 9, 2005 Finding the loops Verify spatial correspond- ence w/ intercon’ing loops

Solar-B Science MeetingKyoto, Nov. 9, 2005 Interconnecting loops: A catalog total loops 43 loops identified 1 st loop: (probably)interconnects definitelyinterconnecting loop flurry ~9:00 171A intensity

Solar-B Science MeetingKyoto, Nov. 9, 2005 Magnetic Model Identify distinct regions with |B z | > 45 G SoHO MDI movie

Solar-B Science MeetingKyoto, Nov. 9, 2005 Magnetic evolution

Solar-B Science MeetingKyoto, Nov. 9, 2005 Coronal Field Inter-connecting flux: Potential field: Increasing Increasing interconnection Increasing AR9574 P051

Solar-B Science MeetingKyoto, Nov. 9, 2005 Flux in 171A loops Assumptions 1.Each loop is a field-line bundle (flux tube) 2.Loops/flux tubes : x-section 3.Loop tracks flux tube for entire life 4.No flux tube re-appears in 171 A

Solar-B Science MeetingKyoto, Nov. 9, 2005 Flux in 171 A loops 1. Each loop is a field-line bundle (flux tube)

Solar-B Science MeetingKyoto, Nov. 9, 2005 Flux in 171 A loops Cummulative loop areas Flux if B 0 = 120 G Y Flux in pot’l model d A =  (d/2) 2

Solar-B Science MeetingKyoto, Nov. 9, 2005 Reconnection observed 24 hour delay Reconn’n burst Mx/sec Heating ~ 5 x erg/sec emergence Dy = Mx 0.1 GV 1 GV

Solar-B Science MeetingKyoto, Nov. 9, 2005 Heating then cooling Yohkoh SXT Hot (~7.5 MK) after reconnection… Cool into TRACE pass-band TRACE 171 A EM T  ~ 10 hrs

Solar-B Science MeetingKyoto, Nov. 9, 2005 The story of the loops density lower bounds radiative cooling time (upper bound on life) life time  heating RTV equilibria

Solar-B Science MeetingKyoto, Nov. 9, 2005 Model of energy storage Constrain Flux Y & minimize energy… 0 W fce W pot W DWDWDWDW Flux Constrained Equilibrium (Longcope 2002)  W ~ ergs

Solar-B Science MeetingKyoto, Nov. 9, 2005 Consequence of latency GOES 1-8 A GOES A Radiated power P ~ 5 x erg/sec Radiated energy ergs D W FCE = 10 31

Solar-B Science MeetingKyoto, Nov. 9, 2005 Role(s) of Current Sheet Site of localized reconnection Mx of newly reconnected flux (1% of DY )

Solar-B Science MeetingKyoto, Nov. 9, 2005 Role(s) of Current Sheet Mx of newly reconnected flux (1% of DY ) Releases D E ~ I Dy ~ ergs

Solar-B Science MeetingKyoto, Nov. 9, 2005 Role(s) of Current Sheets 0 W fce W pot W DWDWDWDW Energy storage: W accumulates for 24 hrs. prior to reconn’ burst Rapidly released via local process

Solar-B Science MeetingKyoto, Nov. 9, 2005 Summary 1.AR 9574: unambiguous reconnection 2.Reconnection in brief (6 hour) burst after delay of ~24 hours 3.Separator reconnection 4.Trigger? … No evidence in p-sphere 5.Produces scores of ~10 18 Mx loops 6.Observed flux accounts for 10% - 30% of maximum allowed (partial reconnection)

Solar-B Science MeetingKyoto, Nov. 9, 2005 Case study: AR 9574 SoHO MDI White light Line-of-sight B 2001 Aug 11, 11:15 UT

Solar-B Science MeetingKyoto, Nov. 9, 2005 Case study: AR 9574 SoHO MDI White light Line-of-sight B AR9570 AR Aug 11, 11:15 UT

Solar-B Science MeetingKyoto, Nov. 9, 2005 Case study: AR 9574 SoHO MDI White light Line-of-sight B AR9570 AR9570 AR9574 AR Aug 11, 11:15 UT

Solar-B Science MeetingKyoto, Nov. 9, 2005 The emergence process whiteblack white black :51 UT :39 UT

Solar-B Science MeetingKyoto, Nov. 9, 2005 Interconnecting loops: A catalog properties of all 43 loops density lower bound

Solar-B Science MeetingKyoto, Nov. 9, 2005 Model of energy storage Unconstrained minimum: Flux Y=Y (v) linking poles 0 W pot W

Solar-B Science MeetingKyoto, Nov. 9, 2005 Steady Reconnection? = 4 months Sweet-Parker:

Solar-B Science MeetingKyoto, Nov. 9, 2005 Comparison of scales Sweet-Parker: c/ w pi riririri

Solar-B Science MeetingKyoto, Nov. 9, 2005 The story of the loops Yohkoh SXT TRACE 171 A 950,000 K ~3,000,000 K movie Loops are hot (~3MK) after reconnection… Gradually cool into TRACE pass-band (All of them?)

Solar-B Science MeetingKyoto, Nov. 9, 2005 Coronal Field State of least energy: Potential Field

Solar-B Science MeetingKyoto, Nov. 9, 2005 Coronal Field Includes connections AR9574 to AR9570 (P051  N01) …all under separatrix surface

Solar-B Science MeetingKyoto, Nov. 9, 2005 Separatrices enclose loops

Solar-B Science MeetingKyoto, Nov. 9, 2005 Coronal Field Inter-connecting lines enclosed by separator

Solar-B Science MeetingKyoto, Nov. 9, 2005 Model of energy storage Lowest Energy w/ fixed Y: Flux Constrained Equilibrium (Longcope 2002) Current-free Current-free except … except …

Solar-B Science MeetingKyoto, Nov. 9, 2005 Model of energy storage Flux Constrained Equilibrium (Longcope 2002) Current-free Current-free except … except … Current Sheet Current separator I ( DY ) I ( DY ) Mag. Energy Mag. Energy in excess of in excess of potential potential D W( DY ) D W( DY ) Lowest Energy w/ fixed Y:

Solar-B Science MeetingKyoto, Nov. 9, 2005 Reconnection observed Y Flux in pot’l model 24 hour delay Incompletereconnection Burst of reconnection Mx/sec = 100 MV

Solar-B Science MeetingKyoto, Nov. 9, 2005 X-ray emission Reconnection burst? GOES 1-8 A