Publications in Comparative Magnetospheres
• Siscoe, G. L.: Towards a comparative theory of magnetospheres, in Solar System Plasma Physics, Vol. II, edited by C. F. Kennel, L. J. Lanzerotti, and E. N. Parker, North-Holland Publishing Co., 299-402, 1979.
• Lanzerotti, L. J., and S. M. Krimigis: Comparative magnetospheres, Physics Today. 38, 24-32, 1985.
• Vasyliunas, V. M.: Comparative magnetospheres: Lessons for Earth, Advances in Space Research, 33, 2113-2120, 2004.
• Blanc, M., R. Kallenbach, and N. V. Erkaev: Solar system magnetospheres, Space Science Reviews, 116, 227-298, 2005.
• Russell, C. T.: New horizons in planetary magnetospheres, Advances in Space Research, 37, 1467-1481, 2006.
Comparative CME and Magnetosphere PhenomenaMagnetosheath
• Draping• Turbulence• Accretion/reconnection
ICME/Magnetosphere• In-transit cooling • interchange reconnection
CME/Plasmoid Dynamics• Acceleration & propagation
Close-Field-Line Heating• Flares and ring current
Eruption Dynamics• Reconnection instability
scenariosEnergetic Particles
• Shock acceleration• Reconnection acceleration
Plasmoid-Like Structures• BBFs• Solar wind examples• Reconnection in solar wind
Pre-Eruption• Flux cancellation for CMEs &
flux buildup for substorms
Eruption• Instability mechanisms for
CMEs and substorms
Post-Eruption• Heating on closed field lines• Current sheets and blobs• CME/plasmoid acceleration and
propagation• In-transit cooling and magnetic
transfiguration
Particle Energization• Reconnection and shock
models
Sheath Phenomena• Draping, turbulence, accretion
and reconnection
Comparative CME and Magnetosphere Phenomena
Reconnection in Solar Corona and Geotail
Same absolute scale in both pictures
Draping in Terrestrial & ICME Magnetosheaths
ICME
E14
00deg
W11
ICME
10
Ho
urs
W02
Kaymaz and Siscoe 2006
Dawn-Dusk Asymmetry in |B|Model and IMP 8 Data Compared
Weak field on dawn side
B (nT)
EastFlankWeak
WestFlank
Strong
1.3
AU
Lat = 10o
East-West Asymmetry in |B|
In ICMEs
CCMC-Cone Model
WANG ET AL.: GEOEFFECTIVE HALO CMES (2002) ZHANG ET AL. SOLAR SOURCES OF MAJOR GEOMAGNETIC STORMS (2003)
Westside CMEs More Geoeffective
Top View Front View
Dawn-Dusk Draping Asymmetry in IMF Bz
0 1 2 3 4 5
nT
|Bz|
Boundary of Body
B (nT) Blat (nT)
East Flank
Strong
EastFlankWeak
WestFlankWeak
WestFlank
Strong
1.3
AU
Lat = 10o Lat = 20o
East-West ICME Draping Asymmetry in IMF Bz
Approx. Boundaryof Disturbed Solar Wind
Blat (nT)
1 AU
Longitude (deg)
Latit
ude
(deg
)
East Flank
Strong
WestFlankWeak
East-West ICME Draping Asymmetry in IMF Bz
Siscoe, MacNeice and Odstrcil 2007
0o
45o
90o
135o
180o
BowShock
Magnetopause
0o
45o
90o
135o
180o
BowShock
Magnetopause
Magnetosheath Accretion
IMF clock angle
Computed Field Strength on StagnationStreamline inEarth’s Magnetosheath(no accretion)
Measured Field Strength Near StagnationStreamline inICME Magnetosheaths(accretion)
Magnetosheath Accretion
Similar CME and Substorm Eruption Scenarios
ThermalBlast
DynamoTether
ReleaseIMF
Connec.Recon.
Inst.Config.
Inst.Current.
Inst.Mass
Exchng.MICInst.
Triggered.Diseqlib.
Directly Driven Blocking-Release
Drc
tly
Drv
nB
lock
ing
-Rel
ease
Dis
-eq
lb.
TetherStraining R
CME
SUBSTORMTether
Straining BMass
Loading
Disequilib.
Substorm CME
Example
Melon-Seed Magnetic Geometry
Forbes
Mikic and Linker
LowZhang
Forbes’ Model
Bo
Ba
2 4 6 8 10246810
Ba=8 G
6 G
4 G
2 G
1 G
0.1 G
Speed (km/s)
Bo=10 G, Density Ratio=1, Cd=0
Distance from Sun Center (Rs)
500
1000
1500
2000
Distance from Sun Center (Rs)
Bo=20 G
15 G
10 G
6 G
Ba=5 G, Density Ratio=1, Cd=0
Velocity Profiles Obtained with Melon-Seed Model
1313
Cliver et al. (1990)Owens et al. (2005)
Elliott et al. (2006)
Av
e N
um
be
r D
en
sit
y a
t 1
AU
(c
m-3)
ICME Speed at 1 AU (km/s)
(a)
(d)(c)
(12.4, 12.9)(25.5, 26.4)
Gopalswamy et al. (2001)
Initial CME Speed (km/s)
Me
an
Ac
ce
lera
tio
n t
o 0
.76
AU
(m
/s/s
)
(b)
*
*
**
(65.2, 64.7)
Bo (G) Ba/Bo Density Ratio
Speed (km/s) Density (cm-3)
Green Circle
40 0.9 0.26 887 1.0
Turquoise Circle
25 0.9 0.3 754 1.5
Red Circle 15 0.8 0.4 693 1.8
Orange Circle
5 0.8 0.5 516 4.5
Purple Square
20 0.3 1.0 678 2.0
Purple Diamond
30 0.11 2.0 634 2.3
Purple Cross 40 .065 3.0 628 2.5
Green Cross 15 0.33 3.0 827 9.4
Red Asterisk 15 0.53 2.0 649 2.3
Forbes CME
Hones TPE
Slavin et al. 1985
0 50 100 150 200
200
400
600
800
1000
Distance from Sun (Rs) and Earth (Re)
Vel
oci
ty (
km/s
)
InterplanetaryCME
GeotailPlasmoid
Pre-Eruption• Flux cancellation for CMEs & flux
buildup for substorms
Eruption• Instability mechanisms for CMEs
and substorms
Post-Eruption• Heating on closed field lines
• Current sheets and blobs• CME/plasmoid acceleration and
propagation• In-transit cooling and magnetic
transfiguration
Particle Energization• Reconnection and shock models
Sheath Phenomena• Draping, turbulence, accretion and
reconnection
Comparative CME and Magnetosphere Phenomena
Pre-Eruption• Forbes/Hughes/Bhattacharjee
Eruption• Forbes/Hughes/Bhattacharjee/
ReevesPost-Eruption
• Raymond/Golub/Korreck/Reeves/Spence
• van Ballegooijen/Hughes• Forbes/Siscoe/Goodrich/Raeder
• Owens/Crooker/Siscoe
Particle Energization• Lee/Schwadron/Korreck
Sheath Phenomena• Farrugia/Smith/Richardson/
Siscoe/Crooker