空间物理学 (I) 2014 年春季学期

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： 63603104Email: miaobin@ustc.edu.cn

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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

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Syllabus of the Space Plasma (II) --by (秋季学期 )

Solar Physics

Magnetosphere Physics

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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%

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Introduction

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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。

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古代对空间现象观测

极光 地磁场

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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)

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1859 年 Carrington 大爆发—A super solar flare

Auroras can be seen at Puerto Rico

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Maunder minimum?

See Eddy, Science 1976

From wiki

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太空时代

Astronaut Buzz Aldrin photographed by Neil Armstrong during the first Moon landing on 20 July 1969

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Space Physics and Astronomy

The bow shock near LL ori

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

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The Sun

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

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Cycle 24?17

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Solar wind

http://solarscience.msfc.nasa.gov/SolarWind.shtml21

ACE: solar wind bulk velocity in 2004

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Corotating Interaction Regions

Schematic illustration of a fast stream interacting with a slow stream [Hundhausen, 1972].

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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.

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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

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Turbulence in the solar wind and magnetic field

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W H Matthaeus

Presentation to the Solar and Heliospheric Survey Panel, 200127

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

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Shock and shock acceleration

Shocks in SpaceShocks in Space Solar Atmosphere

Flares CMEs

Solar Wind Planetary bow

shocks Interplanetary

shocks Coronal Mass

Ejections Corotating

Interaction Regions Termination shock Cometary Shocks

Supernova shocks29

• Galactic Cosmic Rays (GCRs)

Anomalous Cosmic Rays (ACRs)

Solar Energetic Particles (SEPs)

Energetic Storm Particles (ESPs)

Corotating Interaction Regions (CIRs)

Planetary Bow shocks

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New “Bubble” like model, Science, 200932

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

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Stellar system

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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.

大陵五（英仙座 β ）

Galaxy

Mobile phone by Samsung?

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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

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）

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火星表面

空间物理和行星科学

Solar wind and Mars

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The Mars’ bow shock

http://rosetta.jpl.nasa.gov/dsp_images_mars.cfm39

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

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Fig. 11 Treumann and Scholer (2001, The century of Space Science)

n

n

VSW

The Earth’s bow shock and energetic particles

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Geostationary Earth Orbit

Magnetopause

Bow Shock

By S.M. Petrinec, Lockheed Martin 42

The Earth’s magnetosphere

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http://www-spc.igpp.ucla.edu/ssc/tutorial/magnetopause.html45

reconnection

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Observation

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Method of the observation --imaging

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1024X1024 2048X2048 4096X4096

SOHO STEREO SDO

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Method of the observation – in-situ measurement

CODIF

HIA

FGM

Bulk velocity

Density

Pressure

Cluster 离子和磁场的测量51

Space mission

对地观测卫星 地球系统卫星 日地系统卫星 行星探测卫星 日球层探索卫星 天文卫星

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Earth System Science Pathfinder

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ACE 探测仪器

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研究空间物理的理论方法 ?

单个带电粒子的运动； 磁流体力学； 结合统计力学的方法。

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数值模拟

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plasma densityplasma pressure

Forinski 2011

Level 4 Level 5 Level 6

Concentric radial stepping

Areas and edge lengths calculatedfrom spherical trig

Cell areas differ by less than 10%

Forinski 2011

Space Weather

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Solar X-ray flux

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地磁暴（ Geomagnetic storm ）

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Summary

阐述了开展空间物理研究的必要性；

对空间物理的研究对象作了简单介绍，在今后的章节中将作较详细的讨论；

简要介绍了空间物理观测的方式、理论和数值模拟。

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