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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