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 substormsEruption

• 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

transfigurationParticle 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 Hours

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 A

U

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 A

U

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 Dynamo Tether

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 G10 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)

Ave

Num

ber D

ensi

ty a

t 1 A

U (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)

Mea

n A

ccel

erat

ion

to 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)

Velo

city

(km

/s)

InterplanetaryCME

GeotailPlasmoid

Pre-Eruption• Flux cancellation for CMEs & flux

buildup for substormsEruption

• 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

transfigurationParticle Energization

• Reconnection and shock modelsSheath Phenomena

• Draping, turbulence, accretion and reconnection

Comparative CME and Magnetosphere PhenomenaPre-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