study of cme propagation in the inner heliosphere · pdf file2) determine the critical forces...
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![Page 1: Study of CME Propagation in the Inner Heliosphere · PDF file2) Determine the critical forces controlling propagation of CMEs in the corona and interplanetary medium](https://reader034.vdocuments.net/reader034/viewer/2022051305/5aa089747f8b9a67178e583c/html5/thumbnails/1.jpg)
DFW, ST SWG, Caltech, Nov07
Study of CME Propagation in the Inner Heliosphere
D. Webb1,2, T. Howard2,4, T. Kuchar1,2, J. Morrill5, D. Odstrcil3 , R. Harrison6, C. Eyles6,7,8, R. Howard5, B. Jackson9 & J. Johnston2
• Overview- Understand CME propagation & kinematics to large distances- Instruments: LASCO, STEREO SECCHI Heliospheric Imagers, SMEI
• Late January 2007 east limb events- Overlap of fields of view; CME Structure/Geometry- Kinematics over 100° range of elongation from Sun
• CME Propagation Modeling; Work in Progress
• Conclusions/Future Work
1 Institute for Scientific Research, Boston College, Chestnut Hill, MA, USA2 Air Force Research Laboratory, Space Vehicles Directorate, USA3 NOAA SWPC & CIRES, Univ. of Colorado, Boulder, CO, USA4 Physics Department, Montana State University, Bozeman, MT, USA5 Space Science Div., Naval Research Laboratory, Washington, D.C., USA6 Space Science and Technology Dept., RAL, Chilton, UK7 Astrophysics and Space Research, University of Birmingham, Birmingham, UK8 Grupo de Astronomía y Ciencias del Espacio, ICMUV, Universidad de Valencia, Spain9 CASS, University of California – San Diego, La Jolla, CA, USA
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DFW, ST SWG, Caltech, Nov07
SECCHI HI Fields of View
Two of primary science objectives for STEREO Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI):
1) Determine the 3D properties of CMEs2) Determine the critical forces controlling propagation of CMEs in the corona and interplanetary medium
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DFW, ST SWG, Caltech, Nov07
24-25 January 2007 CMEsSOHO EIT & LASCO C3
LASCO C324, 18:18
LASCO C325, 08:42EIT Diff.
24, 14:18EIT Diff.25, 07:13
B9 flare, waveCME speed ~700 km/s
C6 flare, strong waveCME speed ~1500 km/s, decelerating.Asymmetric halo
16 hours later
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DFW, ST SWG, Caltech, Nov07
HI-1A CME Movie: 24-25 January
Courtesy:R. Harrison
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DFW, ST SWG, Caltech, Nov07
HI-2A CME: 26 January02:00 – 22:00
Courtesy: R. Harrison
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DFW, ST SWG, Caltech, Nov07
Comparison of HI-As & SMEIFields of View
SMEI “Fisheye” View to 135° Elongation from Sun (+)
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DFW, ST SWG, Caltech, Nov07
Comparison HI-2A & SMEI: Approx. Same Time & Scale on 26 January
Note similarities in CME & comet (McNaught) tail structures.Note extension of CME in SMEI -sweeps to SE.
SMEI: ~04:00
HI-2A: 06:01
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DFW, ST SWG, Caltech, Nov07
Comparison HIA2 & SMEILate on 27 January
HI-2A: 27 Jan 07; 18:01
SMEI: 27 Jan 07; ~17:00
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DFW, ST SWG, Caltech, Nov07
Elongation vs Time Data Along Similar Trajectories
LASCO + SMEI + HI
0
20
40
60
80
100
120
24.5 25 25.5 26 26.5 27 27.5 28 28.5
DoY (2007)
ELO
NG
ATI
ON
SMEI PA = 97SMEI PA = 60LASCOLASCO HaloMissing LASCOHI PA = 70HI PA = 60Linear (LASCO Halo)Linear (LASCO)
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DFW, ST SWG, Caltech, Nov07
xo
It
Bp
a
Lorentz ForceDrag Force
Lorentz Force [Chen 1996]:
⎥⎥⎦
⎤
⎢⎢⎣
⎡+−−⎟
⎠⎞
⎜⎝⎛=
21
218ln 2
2
2
2
2
2 ξ
pa
tt
BB
aR
RMcI
dtRd l
Drag Mechanism: 2 Models
Solar Wind
1. “Snowplow” [Tappin 2006]:
Driving Mechanism:
2. Aerodynamic Drag [Cargill 2004]:
( ))()()(
)()()(
2
2
RvRvRdt
dMtM
RvRvdt
dMdt
Rd
swc
swc
−Ω=
−−=
σ
( )22
2
)()( RvRvCdt
RdswcD −−= γ
CME Propagation Modeling1) T. Howard (et al., ApJ, 2007) Model
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DFW, ST SWG, Caltech, Nov07
CME Propagation Modeling:Both Launched from Limb
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DFW, ST SWG, Caltech, Nov07
CME Propagation Modeling:Both Launched 60° from SC
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DFW, ST SWG, Caltech, Nov07
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DFW, ST SWG, Caltech, Nov07
SMEI Aitoff Skymaps;
28-29 May 2003
HAFv2 ModelSimulation ofWhite Light Emission
Sun et al., SW, 2007
CME Propagation Modeling2) Hakamada-Akasofu-Fry Kinematic Model
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DFW, ST SWG, Caltech, Nov07
CME Propagation Modeling3) ENLIL 3D MHD Model (Odstrcil)
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DFW, ST SWG, Caltech, Nov07
CME-1: 2007-01-24T18:18, S05E90, R=500, V=700 km/sCME-2: 2007-01-25T08:42, S05E90, R=600, V=1500 km/s
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DFW, ST SWG, Caltech, Nov07
CME-1: 2007-01-24T18:18, S05E90, R=500, V=700 km/sCME-2: 2007-01-25T08:42, S05E90, R=600, V=1000 km/s
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DFW, ST SWG, Caltech, Nov07
CME-1: 2007-01-24T18:18, S05E90, R=500, V=700 km/sCME-2: 2007-01-25T08:42, S05E45, R=600, V=1500 km/s
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DFW, ST SWG, Caltech, Nov07
View from Earth
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DFW, ST SWG, Caltech, Nov07
Preliminary Results
• Can observe and track CME fronts from near-Sun to ~100°
• Similar structure & orientation observed in all instruments out to ~40°- LASCO C2/C3, HI-1A + 2A, SMEI
• In January events, HI-1A & SMEI observe single structures/CMEs- Slow CME followed by faster CME: superposition in LoS or merging?- At large elongation-times SMEI observes front likely near Earth;
Second, fast, halo CME or part of merged event?
• Assumptions:- Material moves radially from Sun; Make measurements along same PAs- How material is observed by given instrument along LoS depends on distance
from Sun, distance from the instrument, & Thomson sphere
• HI and SMEI observations are complimentary- HI-1 fills gap between LASCO/COR & SMEI inner camera - HI-2 overlaps with SMEI over 10’s of degrees – improved resolution- Despite areal gaps, SMEI observes entire sky; HI fields centered on ecliptic.
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DFW, ST SWG, Caltech, Nov07
FUTURE WORK
• Compare CME detection capabilities for more events SMEI vs HIs
• Compare e-t plots with kinematic models CME propagation over large distances
Include drag effects, acceleration vs constant speed, launch location, etc.
• Compare CME structure & propagation with ENLIL MHD model
• Determine flow of density & mass over large distances
• Space weather: Use HIA + HIB + SMEI observations to model (3D) propagation to Earth & estimate timing and size characteristics
THE END
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DFW, ST SWG, Caltech, Nov07
Putting All the A-Telescopes Together
04º15 R
24º96 R
65º260 R
90º360 R4R ≈ 1º
Courtesy:R. Howard
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DFW, ST SWG, Caltech, Nov07
Background Solar Wind at Earth
Low-resolution computations driven by WSA/NSO full rotation maps (blue) and observation at Earth (red dots). Contrast between slow and fast streams will be increased in higher-resolution runs; however, general match is good.
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DFW, ST SWG, Caltech, Nov07
Model Fits to 2 PriorLASCO/SMEI Events
3D Reconstructionsof observed LASCO & SMEI structures
Distance (R) vs Position Angle(PA) plots derived from above
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DFW, ST SWG, Caltech, Nov07
Constant speed fromLASCOModel with
only Drag
Event 1 showsnet deceleration;Well fit by eitherDrag model
Model withboth LorentzForce + Drag
Event 2 showsconstant speed;Well fit by Lorentzdriver + Drag
Model Fits to 2 PriorLASCO/SMEI Events