imaging solar coronal structure with trace leon golub, sao trace: isas - 4 feb. 2003
TRANSCRIPT
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Imaging Solar Coronal Structure With TRACE
Leon Golub, SAO
TRACE:http://vestige.lmsal.comTRACE:http://vestige.lmsal.com
ISAS - 4 Feb. 2003
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The SAO Solar-Stellar X-ray Group
• Leon Golub• Jay Bookbinder• Ed DeLuca• Mark Weber• Joe Boyd• Paul Hamilton• Dan Seaton• With results from A. Van Ballegooijen, A. Winebarger
and H. Warren
http://hea-www.harvard.edu/SSXG/http://hea-www.harvard.edu/SSXG/
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The Major Coronal Physics Problems
1. Why is the corona hot?
2. Why is the corona structured?
3. Why is the corona dynamic & unstable?
Emergence of B into the atmosphere,
and response to B.
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Why Use X-rays to Observe Corona?
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Heating & Dynamics in ARs
TRACE sees four (or possibly only three)distinct processes in active regions:
1. Steady outflows in long, cool structures. ◄
2. Transient loop brightenings in emergingflux areas. Also hot & cool material intertwined –May or may not be related to TLBs.3. Steady heating of hot loops (moss). ◄4. Flare-like events at QSLs (or may be coolingevents predicted by 3.).
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Examples of all four
phenomena
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Another example of flows
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TRACE Active Region Observations are not Consistent With Hydrostatic Model
Figure from Aschwanden et al. 2000
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Non-HS Loops are ubiquitous
courtesy H. Warren
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Partial Listing of Recent Papers About Non-Hydrostatic Loops
• Lenz etal 1999, ApJ, 517, L155.• Aschwanden etal 2000, ApJ, 531,
1129.• Winebarger etal 2001, ApJ, 553,
L81.• Schmelz etal 2001, ApJ, 556, 896.• Chae etal 2002, ApJ, 567, L159.• Testa etal 2002. ApJ, 580, in press.• Martens etal 2002, ApJ, 577, L115.• Schmelz 2002, ApJ, 578, L161.• Aschwanden 2002 ,ApJ, 580, L79.• Warren etal 2003, ApJ, submitted.
• Small gradient in filter ratio, high n. • Multithread model (a la Peres etal 1994, ApJ
422, 412), footpoint heating.• Flows and transient events in non-hydrostatic
loops.• DEM spread → const. filter ratio.• More passbands may help.• Large range in thread T for some loops. • Full DEM need at each point.
• Grad T along loops w/flat filter ratio• Contra Martens.• Repeated heating episodes.
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What Needs to be Explained?
• 1. 195A/173A ratio is flat.
• 2. Emission extends too high for hydrostatic loop (this is debated, though).
• 3. Loop density is high by an order of magnitude.
• 4. Apparent flows (and some Doppler shifts measured).
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Active Region 8536
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How isothermal are these loops?
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SUMER Velocities
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Symmetric vs. Asymmetric Heating
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Static vs. Flow Model
Winebarger etal ApJL (2001)Winebarger etal ApJL (2001)
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High-Conductance Model withAsymmetric Heating
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The Effect of High Conductivity
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Footpoints in Transient Heating
1. Initial energyrelease alongcurrent sheet(“spotty”)
2. Footpooint brightening.
3. Evaporation,then post-flareloops.
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Comparison: Evaporative Model vs.TRACE Obs.
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Moss as TR of Hot Loops
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Heating Shut-off vs. Observations
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Hot Material in the Corona
Mg XII Ly-αsuperposed onFe X (log T =6.9 and 6.0)
Consistent with RHESSIdetection of non-thermalelectrons in “quiescent”active regions.
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END PRESENTATION
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March 17, 2000 M1.1: TRACE 1600 Å Movie
Warren & Warshall,ApJL (2001)Warren & Warshall,ApJL (2001)
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March 17, 2000 M1.1: TRACE 1600 Å Images
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March 17, 2000 M1.1: TRACE 1600 Å Light Curves
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TRACE Footpoint vs. BATSE HXR
→HESSI!
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The Solar-B Mission
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The Solar-B Instrument Complement
1. Solar Optical Telescope with Focal Plane Package (FPP)- 0.5m Cassegrain, 480-650nm- VMG, Spectrograph- FOV 164X164 arcsec
2. EUV Imaging Spectrograph (EIS)- Stigmatic, 180-204, 240-290Å- FOV 6.0X8.5 arcmin
3. X-ray Telescope (XRT)- 2-60Å- 1 arcsec pixel- FOV 34X34 arcmin
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XRT vs. SXT Comparison
1. Higher spatial resolution: 1.0” vs. 2.5”
2. Higher data rate: 512kB continuous.
3. Ten focal plane analysis filters.
4. Extended low-T and high-T response.
5. FIFO buffer for flare-mode obs.
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October 24, 2001 XRT CDR Overview/Systems* P. Cheimets-1
Solar-B XRT Flight Design
Front Door andHinge Assembly
Electrical Box
Ascent Vent2 places
Graphite Tube Assembly
Camera
Feed-ThruElectrical
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Science Themes
• Plasma Dynamics• Thermal Structure and Stability• The Onset of Large Scale Instabilities• Non-Solar Objects
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Plasma Dynamics
• Reconnection– loop-loop interaction
– flux emergence
– nano-flares
– AR jets
– macro-spicular jets
– filament eruption
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Plasma Dynamics• Waves
– origin of high speed wind
– tube waves
– coronal seismology
Figures from Nakariakov et al. (1999): decaying loop oscillations seen in TRACE can be used to estimate the coronal dissipation coefficient.
Re ~ 6 x 105 or Rm ~ 3 x 105 , about 8 orders of magnitude less than classical values.
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Thermal Structure/Stability
• Physical Properties– Te, ne, EM
– energetics
– variability timescales
• Multithermal Structure– steady loops
– filaments
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Onset of Large Scale Instabilities
• Emerging Flux Region– twisting/untwisting
– reconnection
• delta Spots– current sheets
– topology changes
• Active Filaments– Te, ne
– local heating
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Non-Solar Objects
• Jupiter
– S VII @ 198
• Nearby RS Cvns
• Galaxy Cluster Halos
• Comets
• Any EUVE source within 1 deg of Sun
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Science Drivers I: Spatial Scales• “Global” MHD Scales
– Active Regions; – granulation scales
• Transverse scales
n
B and j
• Reconnection sites– location– size– dynamics
105 km
103 km
101 - 103 km
<10 km
<10 km
RAM discoveryspace
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Science Drivers II: Time Scales• Loop Alfven time
• Sound speed vs. loop length
• Ion formation times
• Plasma instability times
• Transverse motions
• Surface B evolution times
• ~10 sec
• ~100 sec
• ~1 - 10 sec
• ~10 - 100 sec
• 1 - 100 sec
• minutes - months
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Optics Metric