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Quantifying Reconnection*

Quantifying Reconnection*. Dana Longcope, Dave McKenzie Jonathan Cirtain, Jason Scott Montana State University. * NASA grant NAG5-10489. Prototype * of Solar-B Reconnection Observation. * TRACE SoHO Solar-A GOES. New AR emerges near old AR

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Quantifying Reconnection*

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  1. Quantifying Reconnection* Dana Longcope, Dave McKenzie Jonathan Cirtain, Jason Scott Montana State University * NASA grant NAG5-10489 Kyoto, Nov. 10, 2005

  2. Prototype* of Solar-BReconnection Observation * TRACE SoHO Solar-A GOES • New AR emerges near old AR • Catalog interconnections (EUV/SXR TRACE/Yohko) • Make a magnetic model (LOS M-gram SoHO/MDI) • Interp’ data w.r.t. the model • Learn about reconnection Requires: long series m-grams (low cadence) long series EUV/SXR (hi cadence) T sensitivity 1 - 10 MK Kyoto, Nov. 10, 2005

  3. AR emergence CORONA (TRACE) 7:34 00:00 12:00 00:00 12:00 00:00 Aug 10, 2001 Aug 11, 2001 AR9574 AR9570 PHOTOSPHERE (SoHO/MDI) Kyoto, Nov. 10, 2005

  4. Why this is reconnection* Tsuneta 1996 Reconnected flux Emerged flux 9570 9574 Old flux Baum & Bratenahl 1976 * It is NOT a flare Kyoto, Nov. 10, 2005

  5. Catalog Interconn’ing loops: (Longcope et al. 2005) Synthetic slit separating diff. ARs 5139 images @ 28 sec 7:00 Aug10 – 23:59 Aug11 BG subtracted TRACE 171 images: Kyoto, Nov. 10, 2005

  6. Lots of loops: ~9:00  14:00 Loops are bright features Gen’l bright’g 1st loop: 12:36 Kyoto, Nov. 10, 2005

  7. Finding the loops • Identify peaks • in slit-intensity • loop = fw @ hm 25 22 23 26 24 Kyoto, Nov. 10, 2005

  8. Finding the loops Verify spatial correspond-ence w/ intercon’ing loops Kyoto, Nov. 10, 2005

  9. Magnetic Model movie SoHO/MDI Identify distinct regions with |Bz| > 45 G Kyoto, Nov. 10, 2005

  10. Magnetic evolution Series of m-grams Kyoto, Nov. 10, 2005

  11. Coronal Field Interconnection (PF) Increasing Inter-connecting flux: P051 AR9574 Kyoto, Nov. 10, 2005

  12. Flux in 171 A loops Each loop is a field-line bundle (flux tube) Kyoto, Nov. 10, 2005

  13. Flux in 171 A loops Y Flux in pot’l model A = p(d/2)2 Flux if B0 = 120 G Cummulative loop areas d Kyoto, Nov. 10, 2005

  14. Reconnection observed Heating ~ 5 x 1026 erg/sec 1 GV 0.1 GV Dy = 1021 Mx 24 hour delay Reconn’n burst 1017 Mx/sec emergence Kyoto, Nov. 10, 2005

  15. Heating then cooling GOES 1-8 A Reconnection burst TRACE 171 A loops 3hr cooling 7.5 MK -> 1 MK Kyoto, Nov. 10, 2005

  16. Heating then cooling movie TRACE 171 A GOES 1-8 A Yohkoh SXT SXT filter ratio EM cool ~ 0.3 hrs Hot (~7.5 MK) after reconnection… T t ~ 10 hrs Kyoto, Nov. 10, 2005

  17. Model of energy storage Constrain Flux Y & minimize energy… W Wfce DW Wpot Flux Constrained Equilibrium (Longcope 2002) W ~ 1031 ergs 0 Kyoto, Nov. 10, 2005

  18. Consequence of latency GOES 1-8 A GOES 0.5-4 A Radiated power P ~ 5 x 1026 erg/sec Radiated energy 1031 ergs DWFCE = 1031 Kyoto, Nov. 10, 2005

  19. Role(s) of Current Sheet Releases DE ~ I Dy ~ 1028 ergs 1018 Mx of newly reconnected flux (1% of DY) Kyoto, Nov. 10, 2005

  20. Summary: Reconnection Lessons • AR emergence ==> reconnection (unambiguous case) • Reconnection in brief (6 hour) burst after delay of ~24 hours • Separator reconnection • Produces scores of ~1018 Mx loops • Delayed reconnection ==> storage of energy: 1031 ergs Kyoto, Nov. 10, 2005

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