空间物理学 (I) 2014 年春季学期

1. 空间物理学(I)2014年春季学期 缪彬 （miào bīn） 地球和空间科学学院 办公室：行政科研楼1327 电话：63603104 Email: miaobin@ustc.edu.cn

2. 课程大纲 • Introduction • Plasma • Single particle motion • Introduction of MHD • Introduction of Heliosphere • The Sun • Solar wind • Interplanetary magnetic field • The Earth’s radiation belt • The Earth’s magnetosphere • Ionosphere • Energetic particles • Shock and Shock acceleration • Wave and Turbulence • Reconnection • Observation and instruments • Summary

3. Syllabus of the Space Plasma (II) --by (秋季学期) Solar Physics Magnetosphere Physics

4. 考试形式 • Presentation 从指定文献中选择一篇文章作口头报告（40%）： 要求：15分钟的报告，包括两到三个问题的提问时间。 • Term paper 并且撰写同一篇文献的书面阅读报告（共30%）： 初稿：上交日期 4月21日 （30%，迟交的报告扣10分） 定稿：（最后一次课结束后三天内）（10%） • Homework and Quiz 30%

5. Introduction

6. 空间物理的重要性 • 人类对自然界的探索; • 地理大发现的延伸—太空时代； • 空间天气对人类活动的影响； • 与天文物理的联系。

7. 古代对空间现象观测 极光 地磁场

8. The earlist sunspot records in Han Shu Wuxingzhi (Vol.27, Page 1507) 汉成帝河平元年三月乙未（March 28 BC） “日出黄，有黑气大如钱，居日中央”(Sun rose while appeared yellowish, in the disk center there was a dark spot of coin size) 中国汉代关于太阳黑子的记录 The page is from Dr. Wang, Jingxiu (NAOC)

9. 1859年Carrington大爆发—A super solar flare Aurorascan be seen at Puerto Rico

11. From wiki Maunder minimum? See Eddy, Science 1976

12. 太空时代 Astronaut Buzz Aldrin photographed by Neil Armstrong during the first Moon landing on 20 July 1969

13. Space Physics and Astronomy The bow shock near LL ori

14. 空间物理的研究对象 • The Sun and solar wind • Interplanetary plasma • Heliosphere • Magnetosphere • The Solar-Terrestrial environment

15. The Sun 1. Core2. Radiative zone3. Convective zone4. Photosphere5. Chromosphere6. Corona7. Sunspot8. Granules9. Prominence

17. Cycle 24?

21. Solar wind http://solarscience.msfc.nasa.gov/SolarWind.shtml

22. ACE: solar wind bulk velocity in 2004

23. Corotating Interaction Regions Schematic illustration of a fast stream interacting with a slow stream [Hundhausen, 1972].

24. Magnetic field Steve Suess (NASA/MSFC) prepared this figure, which shows the Sun's spiraling magnetic field from a vantage point ~100 AU from the Sun.

25. Park spiral and heliospherical current sheet Smith et al., Observations of the interplanetary sector structure up to heliographic latitudes of 16 degrees: Pioneer 11, J. Geophys. Res., 83, 717, 1978

26. Turbulence in the solar wind and magnetic field

27. W H Matthaeus Presentation to the Solar and Heliospheric Survey Panel, 2001

28. Flux tube Borovsky, J. E. (2008), Flux tube texture of the solar wind: Strands of the magnetic carpet at 1 AU?, J. Geophys. Res., 113, A08110

29. Shocks in Space Shock and shock acceleration • Solar Atmosphere • Flares • CMEs • Solar Wind • Planetary bow shocks • Interplanetary shocks • Coronal Mass Ejections • Corotating Interaction Regions • Termination shock • Cometary Shocks • Supernova shocks

30. Galactic Cosmic Rays (GCRs) • Anomalous Cosmic Rays (ACRs) • Solar Energetic Particles (SEPs) • Energetic Storm Particles (ESPs) • Corotating Interaction Regions (CIRs) • Planetary Bow shocks

32. New “Bubble” like model, Science, 2009

33. Interstellar medium (ISM) 星际间物质--This matter includes gas in ionic, atomic, and molecular form, dust, and cosmic rays. Radiation （Energy） Magnetic field

34. Stellar system 大陵五（英仙座β） Algol (β Persei) is a triple-star system (Algol A, B, and C) in the constellation Perseus, in which the large and bright primary Algol A is regularly eclipsed by the dimmer Algol B every 2.87 days. This animation was assembled from 55 images of the CHARA interferometer in the near-infrared H-band, sorted according to orbital phase. Because some phases are poorly covered, B jumps at some points along its path.

35. Galaxy A large number of stars bound by gravitation is generally called a star cluster or galaxy, although, broadly speaking, they are also star systems. NGC 4414 Milky Way Mobile phone by Samsung?

36. 太阳风和行星、彗星的相互作用 • 彗星（无磁场）； • 无内禀磁场的行星（火星） • 有内禀磁场的行星（地球）

37. 空间物理和行星科学 火星表面

38. Solar wind and Mars

39. The Mars’ bow shock http://rosetta.jpl.nasa.gov/dsp_images_mars.cfm

40. Bow Shock Density transition from downstream to upstream. The green line is the hyperbolic tangent fit; red vertical lines show the density transition scale [Bale et al., Phys. Rev. Lett. 91, 265004 (2003)]. http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=34927

41. The Earth’s bow shock and energetic particles n VSW n Fig. 11 Treumann and Scholer (2001, The century of Space Science)

42. Bow Shock Magnetopause Geostationary Earth Orbit By S.M. Petrinec, Lockheed Martin

43. The Earth’s magnetosphere

45. http://www-spc.igpp.ucla.edu/ssc/tutorial/magnetopause.html

46. reconnection

47. Observation

48. Method of the observation --imaging

49. SOHO STEREO SDO 1024X1024 2048X2048 4096X4096