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Hinode9 @Belfast 13-18 September 2015 Tracing the release sites of the energy stored in the twisted coronal structure in X-class flares Toshifumi Shimizu (ISAS/JAXA, Japan) & Satoshi Inoue (Max-Plank Institute for Solar System Research, Germany) 2015.9.14 Hinode 9 3 “Eruptive” solar flares ! General scenario Formation of magnetic flux rope Free energy stored as a nonpotential magnetic field in the corona! Non-potential field Active region in Dec 2006 Magnetic Develop MHD dynamically reconnection Destabilization Eruption of magnetic flux rope Filament eruption, CME 2015.9.14 Hinode 9 (Amari+14 Nature) 4 Where and how the energy is stored and released? ! ! 3D non-potential magnetic structure formed in the corona Hinode SOT’s Spectro-Polarimeter (SP) makes the most accurate measurements of vector magnetic fields at the photosphere. = 1000 = 1000 2012/3/6 22UT The boundary condition for deriving 3D coronal magnetic fields with non-linear force free field (NLFFF) modeling (Inoue+14) 2015.9.14 Hinode 9 X5.4 X1.3 5 2012/3/7 X5.4/X1.3 Flare A geoeffective solar flare coronagraph LASCO Magnetic field surrounding the flare core, producing launch of a plasma ejection 870km/s Preflare Onset 30” (20,000km) SDO/AIA 194A (FeXII+FeXXIV) 2015.9.14 10min 6 A strong sheared magnetic configuration White – positive Black - negative Magnetic flux Bz Solar surface: Continuum (Hinode SOT/SP) Yellowed areas – flare ribbons at the beginning of the X5.4 ! A candidate for triggering the X5.4 flare " A small-scale trigger structure identified in the red square 2015.9.14 Hinode 9 7 Surface gas dynamics ! Conditioning the magnetic structure for flare trigger FOV 20”x20” (Shimizu, Lites, & Bamba 2014) = 1000 Trigger field Image: Bz, arrows: (Bx, By) (in local frame) Yellow contours: flare ribbons 2015.9.14 Doppler velocity -5 Km/s 0 Hinode 9 N17E27: ~30 deg tilted from LOS +5 8 Evolution of horizontal magnetic flux Flare onset 2.0 Area size 1.5 1.0 unit: x10 2 ! □ : mag. flux of horizontal field (SP) + : area size of horizontal field (SP) 0.5 mag. flux 0 Dotted: Line-of-sight magnetogram (HMI) 2.5 6 4 3.0 Area size (x107 km2) magnetic flux (x1019 Mx) 8 0.0 18:00 20:00 22:00 00:00 02:00 04:00 Start Time (06-Mar-12 17:00:00) The photospheric magnetic field near PIL becomes more horizontal after eruptions, related to the newly formed low-lying fields during flares 2015.9.14 Hinode 9 9 NLFFF & Twist Map (-1<Tn<0) 3D coronal field from NLFFF modeling Pitch (twist number) of each field line from one footpoint to the other. 2hr before the flare: 22:00 UT on 2012 March 6 Force-free condition 2015.9.14 ∇ × B = αB Hinode 9 Tn = 1 4π ∫ αdl -1 Tn 0 Tn definition from Inoue+12 10 Field twist after the X5.4 flare ! Tn = 1 4π ∫ αdl The magnetic twist was changed with the flare: Decreased, increased, and redistributed. Two hours before the flare onset 22 UT on 6 March Two hours after the flare onset 2 UT on 7 March Tn 0 Twist changes in the two maps Tn = 2015.9.14 Hinode 9 ΔTn ! ! ! ! -1 2015.9.14 ΔTn 1 Hinode 9 -1 11 1 4π ∫ αdl Positive ΔTn: Twist is increased. Negative ΔTn: Twist is decreased. Twist is reduced with the flare at many locations including the location of the flare ribbons at the early phase. Twist is slightly increased mainly at outer area. 12 Chromospheric flare ribbons ! ! Trace which footpoint locations of the magnetic field lines are involved in the energy release each time. One-to-one correspondence of bright kernels in flare ribbons confirms that the coronal field derived with NLFFF is reasonable. SDO/AIA 1600A 2015.9.14 Hinode 9 13 Twist change at the locations swept by flare ribbons Not reliable, affected by the boundary condition in NLFFF Total of changes in magnetic twist at the flare ribbon locations 1-8 0.5-4 ! Total intensity of the flare ribbons (AIA 1600A) (arbitrary unit) The largest decrease was observed in the magnetic field lines involved at early phase of the energy releases. 2015.9.14 Hinode 9 14 Summary ! Some key observational elements for producing flares, discussed with Hinode magnetic-field measurements. – A high-speed gas dynamics at the solar surface for leading to the onset of flares (Shimizu, Lites & Bamba 2014). – The magnetic twist formed in the corona ! ! Magnetic twist is redistributed (decreased and increased) in coronal fields, in response to the occurrence of the X5.4 flare. The largest decrease in magnetic twist was observed in the magnetic field lines involved at early phase of the energy releases 2015.9.14 Hinode 9 15