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Aerospace Environment ASEN-5335

Aerospace Environment ASEN-5335. Instructor: Prof. Xinlin Li (pronounce: Shinlyn Lee) Contact info: e-mail: lix@lasp.colorado.edu (preferred) phone: 2-3514, or 5-0523, fax: 2-6444, website: http://lasp.colorado.edu/~lix

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Aerospace Environment ASEN-5335

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  1. AerospaceEnvironmentASEN-5335 • Instructor: Prof. Xinlin Li (pronounce: Shinlyn Lee) • Contact info: e-mail: lix@lasp.colorado.edu (preferred) phone: 2-3514, or 5-0523, fax: 2-6444, website: http://lasp.colorado.edu/~lix • Office hours: 9:00-11:00 pm Wed at ECOT 534, Tue & Thu, after class. • Read Chapter 1 & 2.

  2. The Earth’s Magnetosphere Energetic electrons and protons are not able to penetrate down to the Earth’s surface directly. Particles gain entry through the cusps that are shaped like funnels over the polar regions or they enter far downstream from the Earth. Particles that enter downstream can be transported toward the Earth and accelerated to high energies, producing auroras and radiation belts.

  3. The flare was an ‘X-class’ and accompanied by one of the largest solar energetic proton events ever recorded c3714

  4. These protons reach Earth in less than 30 minutes Less than 1 hour after the initial proton arrival the POLAR/VIS imager is saturated and remains so for almost a day Vis-proton-bastille

  5. A Schematic View of the Locations of Radiation Belts • Blue: inner belt, >100MeV protons, rather stable • Purple: outer belt, 100s keV and MeV electrons and ions, not stable at all • Slot region in between • Yellow: ACRs, stable • White line: Earth’s magnetic field, approx. by a dipole field

  6. Charged Particle Motions in Earth’s Magnetic Field • Gyromotion motion: =p2/2mB (1st), T_g~10-3 sec • Bounce Motion: J= p||ds (2nd), T_b~100 sec • Drift motion: =BdA (3th) , T_d~103 sec

  7. PARTICLE ENERGIES OF CONCERN

  8. EVA • EVAs - additional radiation exposure concern • Lower shielding • Eye dose • Skin dose • 51.6 degrees, new concern for electron events • One area where we don’t currently have a good model. Have limited measurements outside at our orbits during events from Shuttle and MIR, so we don’t have enough data for any kind of empirical model. • 145 more EVAs are planned for ISS completion

  9. The flare was an ‘X-class’ and accompanied by one of the largest solar energetic proton events ever recorded c3714

  10. ISS ALTITUDE PROFILE

  11. Earth’s Debris Environment • Ground based radar and optical map > 1 cm below 2000 km and > 10 cm above 2000 km • Shuttle surface and window damage for LEO • Need for smaller debris (<10 cm) map in most of space LEO GEO

  12. To Advance observing capabilities fundamental understanding of processes data processing and analysis numerical modeling transition of research into operational techniques and algorithms forecasting accuracy and reliability space weather products and services education on space weather  National Space Weather Program

  13. To prevent or mitigate under- or over-design of technical systems regional blackouts of power utilities early demise of multi-million dollar satellites disruption of communications via satellite, HF, and VHF radio disruption of long-line telecommunications errors in navigation systems excessive radiation doses dangerous to human health National Space Weather Program

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