Transcript Introduction including sylllabus

Solar and Heliospheric Physics
CSI 769
Fall 2009
Jie Zhang
What Physics?
•Magnetism (corona)
•MHD (Magnetohydrodynamics) Physics
•Fluid Physics + Maxwell Equations (EM)
•Magnetic Reconnection
•Particle Acceleration and Transportation
•Not “Plasma Physics”
•Not “Introduction to Space Weather”
•Not “Magnetospheric and Ionospheric Physics”
The Cosmological Context
We are located in
Milky Way Galaxy
28,000 light years
from the center
One of 200 billion
stars in our Galaxy
The Sun: an Ordinary Star
•An ordinary main
sequence star
•5 billion years old
•5 billion years
more to go
Local Interstellar space
Solar wind
creates a big
teardropshaped
heliosphere
around the
solar system,
by interacting
with the
interstellar
wind
Local Interplanetary Space
The Earth
3rd planet from
the Sun
1 AU = 150
million km
Travel time:
By light -8 minutes
By Solar Wind- ~ 100 hrs
What Impacts
•The Sun is the source of energy for life on
Earth
•The Sun (and surrounding heliosphere) is the
best lab for studying our universe
•The Sun is the driving source of Space
Weather, that has adverse effects on
technological system and life on Earth
Space Weather
"Space weather describes the conditions in space
that affect Earth and its technological systems.
Our space weather is a consequence of the
behavior of the sun, the nature of Earth's
magnetic field, and our location in the solar
system”
----National Academy of Science, 1997
Space Weather: the Process
It starts
from an
eruption
from the
Sun.
Prediction
depends on
how it
propagates
Space Weather: effects
Aurora; Geomagnetic Storm
From Space
Space Weather: effects
An adverse effect
Power failure due to
March 1989 storm
Damaged transformer
Space Weather: effects
On Human Space Exploration
On crew and
passengers of
polar-route
airplanes
Space Weather: effects
On Satellite Operation
Space Weather: effects
On Communication and Navigation
Space Weather: the Systems
The Source of the Energy?
Planet
Magnetic energy through magnetic field
generated by solar dynamo, which has 11-year
solar cycle
Solar Cycle
(SOHO/MDI)
Storage of Energy?
Planet
Energy stored and released in magnetic field
TRACE
PFSS Model
Release of Energy: Flares
Planet
GOES/SXI
RHESSI & TRACE
Release of Energy and the
driver?
Planet
Coronal mass ejections
SOHO/LASCO/C2
CME in Interplanetary Space
STEREO/
SECCHI/HI-1
CME Simulation (Credit: Odstrcil)
On Satellite Operation
Heliosphere: solar wind
Planet
Spiral solar wind magnetic field: radial motion
of solar wind combined with Sun’s rotation
Sprinkler
Analogy
Magnetosphere
Planet
A cometshaped
region
around the
Earth
Magnetosphere: Simulation
Planet
Magnetosphere
Planet
Electric
Currents in
Magnetosphere
Magnetosphere
Planet
Energetic
particles in
Van Allen
radiation
belt
Ionosphere
Planet
Density fluctuation affects radio wave
reflection and transmission
Neutral Upper Atmosphere
Planet
It is coupled with ionosphere
Now, the golden age!
HINODE
Now, the golden age!
STEREO
Now, the golden age!
SDO
Now, the golden age!
•The stunning new observations
•More importantly, the mind-opening
observations, which provide the instinct
insight for scientific understanding
•Advancing in theory
•Advancing in computer modeling and
computational data processing
•Most importantly, your knowledge of physics
principles - what this class cares most!
The Syllabus
Content
1. Introduction/Overview: Solar Physics and Space Weather
2. MHD Equations including Maxwell Equations
3. Solar Magnetism 1: Potential Field, Force Free Field
4. Solar Magnetism 2: Helicity, Separators
5. Magnetic Reconnection 1: Current Sheet
6. Magnetic Reconnection 2: Magnetic Annihilation
7. Magnetic Reconnection 3: Steady Reconnection
8. Magnetic Reconnection 4: Unsteady Reconnection
9. Solar Applications: Models of CMEs and Flares
10. Solar Applications: Models (student presentation)
11. Heliosphere and Solar Wind
12. Shock Formation and Particle Acceleration
13. ICMEs and Magnetic Clouds
Text Book
•
Required:
1. Magnetic Reconnection - MHD Theory and Applications
–
By Eric Priest and Terry Forbes
•
Supplement:
1. Physics of the Solar Corona
•
By Markus Aschwanden
2. An Introduction to Plasmas and Particles in the
Heliosphere and Magnetosphere
–
By May-Britt Kallenrode
3. Online Resources
Assignments
•
Homework
– ~ weekly homework
•
Project
– Proj 1: PFSS model calculation
– Proj 2: pick one from the following two options
•
•
Observing CME/flare Initiation (SDO)
Observing CME Propagation (STEREO)
Grading
•
•
•
•
Homework
Projects
One mid-term
One final
(25%)
(30%)
(20%)
(25%)
Contact
• Instructors: Prof. Jie Zhang
• Contact Info: [email protected] (e-mail)
1-703-993-1998 (phone)
• Office Hour: 2:00 PM to 3:30 PM, Thursday
or by appointment
• Office:
Room 351, Research Bldg 1
The End