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Space weather презентация
Содержание
- 1. Space weather
- 2. Coronal loops Intense magnetic field lines trap plasma http://www.nasa.gov/centers/goddard/images/content 203911main_TRACE_loop_arcade_lg.jpg
- 3. Coronal mass ejection Explosive ejection of
- 4. Normal conditions Typical concentration of particles
- 5. During a solar flare, particle flux increases by a factor > 100,000
- 6. Ionized radiation is bad for you… Sievert
- 7. Multiply rem x 10 to get mSv Solar Flare Ionized radiation is bad for you…
- 8. Fukashima Reactor #1 500 uSv/hr
- 9. Interaction of the solar wind and Earth’s
- 10. But the solar wind cannot cross fields lines, so what happens?
- 11. Bow shock – where velocity of solar
- 12. The polar auroral fountain sprays ions -
- 13. The magnetic conditions inside and outside the
- 15. The solar current sheet (or magnetic equator)
- 16. Some small amount of charged particles can
- 17. Go to notes on electron orbits in magnetic fields….
- 19. Aurora Borealis (northern lights)
- 20. From space
- 23. Van Allen radiation belts Outer belt: 4
- 24. 1800 180 18 mSv/hour
- 25. Multiply rem x 10 to get mSv 1 hour in Van Allen Belt
- 26. The South Atlantic Anomaly SAA is the
- 27. Magnetic fields on other planets…. Saturn sometimes sits within Jupiter’s magnetosphere
- 28. Jupiter’s radiation belt (Jupiter’s magnetotail extends beyond Saturn)
- 29. Aurora on Jupiter
- 30. Io is a major source of plasma- Sulphur dioxides photo dissociates… Jupiter’s northern lights
- 31. Saturn too…
Coronal loops Intense magnetic field lines trap plasma http://www.nasa.gov/centers/goddard/images/content 203911main_TRACE_loop_arcade_lg.jpg
Слайд 2Coronal loops
Intense magnetic field lines trap
plasma
http://www.nasa.gov/centers/goddard/images/content 203911main_TRACE_loop_arcade_lg.jpg
Слайд 4Normal conditions
Typical concentration of particles near Earths ~1 particle / cm3
Typical
velocity ~400 km/sec;
(Protons)
Слайд 6Ionized radiation is bad for you…
Sievert – measure of radiation energy
absorbed (in gamma ray equivalent)
(joules per kg)
(joules per kg)
Слайд 9Interaction of the solar wind and Earth’s magnetic field
All else being
equal, this is what the Earth’s field would
look like from far away
look like from far away
Слайд 11Bow shock – where velocity of solar wind drops sharply as
it approaches the magnetopause
Magnetopause – delimits boundary between solar wind and Earth’s magnetosphere.
Magnetosheath – region between the bow shock and the magnetopause
Outside the bow shock the solar wind wins, Inside the magnetopause the Earth’s field wins,
in between is a messy competition
Magnetopause – delimits boundary between solar wind and Earth’s magnetosphere.
Magnetosheath – region between the bow shock and the magnetopause
Outside the bow shock the solar wind wins, Inside the magnetopause the Earth’s field wins,
in between is a messy competition
Слайд 12The polar auroral fountain sprays ions - oxygen,
helium, and hydrogen
- from Earth's upper ionosphere
into deep space. The loss is miniscule compared to
the immense ocean of air covering our world, but is
significant in terms of what drives space weather around our world.
into deep space. The loss is miniscule compared to
the immense ocean of air covering our world, but is
significant in terms of what drives space weather around our world.
http://science.nasa.gov/
Слайд 13The magnetic conditions inside and outside the
Earth’s magnetosphere are very
different
Much quieter inside
Слайд 14
Generation of a current sheet in the magneto-tail.
Occurs where the magnetic
field switches from south to north, and the field lines are stretched out by the solar wind
Circles show the sense of the magnetic field around parallel wires
(with current into page). For a ‘sheet’ of current, the magnetic field
Would be given by the red and green lines.
Слайд 15The solar current sheet (or magnetic equator)
Controlled by off-axis dipole, and
~27 day solar rotation.
Magnetic equator precesses; from Earth it appears to oscillate
up and down
Magnetic equator precesses; from Earth it appears to oscillate
up and down
Слайд 16Some small amount of charged particles can enter magnetopause where field
lines and particle trajectories are most nearly parallel
Слайд 23Van Allen radiation belts
Outer belt: 4 to 5 Re, electrons
Inner belt:
0.01 to 1.5 Re, protons, α particles
Слайд 26The South Atlantic Anomaly
SAA is the closest approach of Van Allen
radiation belt to the surface.
Happens b/c magnetic pole is tilted relative to Earth’s axis, and b/c Earth’s magnetic field is not uniform
If you are an astronaut or a satellite you want to avoid the area (Hubble shuts down).
SAA is drifting westward ~0.3o per year
Happens b/c magnetic pole is tilted relative to Earth’s axis, and b/c Earth’s magnetic field is not uniform
If you are an astronaut or a satellite you want to avoid the area (Hubble shuts down).
SAA is drifting westward ~0.3o per year
