月球表面反射太陽風質子之粒子模擬

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姓名

李倩敏(Chien Min) 查詢紙本館藏

畢業系所

太空科學研究所

論文名稱

月球表面反射太陽風質子之粒子模擬
(Test Particle Simulations of Reflected Solar Wind Protons from the Lunar Surface)

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摘要(中)

繼日本近年的探月計畫-KAGUYA首次發現少量的太陽風粒子能夠從月球表面反射出來後，我利用單一粒子模擬計算太陽風質子與月球日側半球的交互作用。計算結果發現在距離月球表面一百公里高的球層，反射質子的分佈呈現明顯的南北與東西向不對稱性，這是因為質子從表面反射後受到電場加速，而具有相當大的迴旋半徑，並且其移動方向又受到行星際間磁場和電場的方向所影響。計算結果也指出，反射質子在接近月球表面的區域就能被行星際間電場加速到高速，我們稱之為Self-pickup過程。在特定的行星際磁場強度下，從表面反射出來的質子有機會進入月球的夜側半球，這是個以往被認為缺乏太陽風質子的空腔區域。

摘要(英)

Following the first discovery of reflected solar wind protons from the lunar surface by KAGUYA experimental team, I study the motion of the solar wind protons which are reflected from the lunar dayside hemisphere by using single particle trajectory calculations in a Monte-Carlo simulation. The global distribution of these reflected protons at 100 km altitude above the lunar surface shows strong asymmetry in north-south and dawn-dusk directions because of their large gyroradii and the directions of the accelerating electric field and the interplanetary magnetic field. The reflected protons could be accelerated to high speed in near-surface region because of the self-pickup process. Under certain condition of the interplanetary magnetic field, a portion of them can reach the shadow region which is usually considered to be devoid of solar wind protons.

關鍵字(中)

★ 粒子模擬
★ 太陽風
★ 月球

關鍵字(英)

★ lunar surface
★ Moon
★ solar wind
★ particle simulation

論文目次

Chapter 1. Introduction 1
Chapter 2. Basic Equations and Model Settings 7
2.1 Basic Equations and Parameters 8
2.2 Model Settings 10
Chapter 3. Simulation Results 14
3.1 Trajectories of Reflected Solar Wind Protons 15
3.2 Energy Distribution Along Latitudes 22
3.3 Global Distribution of Flux and Energy 26
3.4 Lunar Wake Boundary Electric Field 34
Chapter 4. Discussions and Summary 38
Appendix 1: Lunar Surface Charging 40
Appendix 2: Lunar Magnetic Field Anomaly 42
Bibliography 43

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指導教授

葉永烜(Wing-Huen Ip)

審核日期

2010-6-30

推文