1 / 56

Problems in Space Physics

Problems in Space Physics. 長井嗣信 東京工業大学. 磁気圏の未解決問題 「いつも同じ話をしている」 容易に解決できそうだが 何が観測的に問題なのか ３．今後どうすべきか. Substorm Onsets Magnetic Storms Plasma Convection. Substorm Onsets Global Images Intense Ground Observation Network Mid-Tail Observations 10-30 Re

gurit
Download Presentation

Problems in Space Physics

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Problems in Space Physics 長井嗣信 東京工業大学

  2. 磁気圏の未解決問題 • 「いつも同じ話をしている」 • 容易に解決できそうだが • 何が観測的に問題なのか • ３．今後どうすべきか

  3. Substorm Onsets • Magnetic Storms • Plasma Convection

  4. Substorm Onsets • Global Images • Intense Ground Observation Network • Mid-Tail Observations 10-30 Re • Geosynchronous Orbit 6.6 Re

  5. L. A. Frank ICS-4 (1998) 0726 UT January 12, 1997

  6. Polar/UVI by A. Ieda 0725:11 UT

  7. Polar/UVI January 12, 1997 0724:54 UT

  8. 0725 UT

  9. 0725 UT

  10. 0723 UT

  11. Gang Lu JGR 1999

  12. 70 Gang Lu JGR 1999 70

  13. SIT-TV at Syowa 427.8 nm Kadokura (2002)

  14. Problems 1. Spatial Resolution 2. Time Resolution 3. UV 4. Magnetic Field Tracing 5. Conjugate Events

  15. L. R. Lyons et al. JGR 2001

  16. L. R. Lyons et al., JGR 2001

  17. Geographic Longitude Geomag. Lat. 1.5 -8.3 -10.4 10E 71.3 E 105E -8.7 -1.1 8.6 141 E 192.5 E 322.5E

  18. Global Satellite Aurora Images Spatial Resolution Time Resolution UV Comparison with Ground Observations Geosynchronous Substorm Signatures Longitudinal Effect Particles or Magnetic Field

  19. McPherron 1991 Kamide and Baumjohann 1993

  20. 2. Magnetic Storms Burton et al., 1975

  21. Ring Current Modeling Ebihara et al. 2001, 2002

  22. Strangeway and Johnson 1983

  23. Strangeway and Johnson 1983

  24. Strangeway and Johnson 1983

  25. Magnetic Storms • Solar wind parameters Dst • Ring current modeling (dipole field) Dst • H+ vs. O+ • What should be known? • Particle distributions • Time, Position (L, MLT, Latitude) • Energy, Species

  26. 3. Plasma Convection • Plasma Transport = Field Transport Pictures from Ground Observations Pictures from Tail Observations

  27. Polar Cap Potential Drop 100 kV Polar Cap > 75 degrees L = 2 x 3.14 x 6371.2 x 30/360 = 3300 km E = 100kV / 3300km = 30 mV/m B = 60000 nT V = E/B = 30 mV/m / 60000 nT = 500 m/s T = 3300km / 500 m/s = 100 min Vsw = 500 km/s T = 100 Re/500 km/s = 20 min

  28. Nishitani et al. JGR 2001

  29. Plasma Convection in the Tail Stationary vs Bursty Paterson et al. JGR 1998 Angelopoulos et al. 1999 100 Re/10 km/s = 1000 min

  30. A dipolarization at 10 Re (for a substorm)

  31. Mid- and Near-Tail Plasma Observations • Plasmas are NOT MHD • Problems in the Present Instruments No Convincing Observations

  32. 今後の方向 • 確かに進歩 • 新たな問題 • 根本的な問題 • 将来計画 • 対象の明確化（絞込み） • 何が必要とされているか • 対象にあった観測　機械と軌道

  33. 4. IMF Bz Control for the Plasma Sheet • IMF Bz > 0 (northward) • IMF Bz < 0 (southward) • ssc (density increase in SW)

More Related