Forbes CME

Hones TPE

5 10 15 20

50

100

150

200

250

300

Distance in Rs

Acc

eler

atio

n (

m/s

2)

CME Acceleration

50 100 150 200

200

400

600

800

1000

1200

So

lar

Win

d S

pee

d (

km/s

)

1 A

U

Solar Wind Profile

CME VelocitySlavin et al. 1985

40 60 80 100

50

100

150

200

250

300

Acc

ele

ratio

n (

m/s

/min

)

Distance from Earth (Re)

Plasmoid Acceleration

40 60 80 100

200

400

600

800

Plasmoid Velocity

Distance from Earth (Re)

Ve

loci

ty (

km/s

)

50 100 150 200

250

500

750

1000

1250

1500

Ve

loc

ity

(k

m/s

)

Distance from Sun (Rs)

ICME (km/s)

X ray bright points

Solar active regions

G,K & M dwarfs

T Tauri stars

Convective envelope

Pevtsov et al., 2003

“It cannot be emphasized too strongly that the development of a solid understanding of the magnetic activity, occurring in so many forms in so many circumstances in the astronomical universe, can be achieved only by coordinated study of the various forms of activity that are accessible to quantitative observation in the solar system.”

E. Parker Cosmical Magnetic Fields

A Need for a Science of Heliophysical Plasmas

Ingredients of a NESSC Comparative Study of

Explosive Energy Conversions

1. CME/substorm initiation2. ICME/plasmoid transport3. Roles of magnetic reconnection (pre-

explosion, explosion, post explosion)4. Particle heating and acceleration5. Flares and auroras6. Your thoughts here7. And here