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List of Tables 2.1 2.2 3.1 Summary of the instrumental parameters for the new version of the Fabry- Perot Doppler Imaging System (FPDIS) List of the optical components used for the FPDIS. Summary of Fabry-Perot Doppler Imaging observations at Syowa station, Antarctica from March to September, 1994. The symbol 'o' in the column of condition indicates that full observation was made, while the symbol 'A' indicates that observation was made partially. The notation E Kp Pre/Next represents the summation of Kp values on the day of observation start and the next day. 32 34 53
Chapter 1 Introduction 1.1 The Earth's thermosphere The Earth's thermosphere is defined as the high temperature region extending from the mesopause located at an altitude of 80-90 km to the thermopause located at an altitude of 300-500 km. The temperature increases rapidly with height in the lower thermosphere, and becomes asymptotic to a value of the order of 1000 K in the upper thermosphere. The fundamental structure of the thermosphere is determined by a balance of heating and cooling. The thermosphere is characterized by a coexistence of neutral gases and ionized gases and thus the dynamics of this region is governed by a combination of physical and chemical processes of the neutral gases and electrodynamical processes of the ionized gases. These interactive processes were reviewed by Hunsucker [1982], Foster and St.-Maurice [1983], Rees et al. [1983], Killeen [1987], Crowley [1991], Solomon [1991], and Tithcridge [1995]. Figure 1.1 shows a scheme of thermospheric phenomena and physical processes. Of various thermospheric heat sources, solar extreme ultraviolet (EUV) and ultraviolet (UV) radiation is the most important source in a globally-averaged sense, and it is primarily responsible for maintaining high thermospheric temperature and for producing a pressure- gradient force that drives a fundamental day-to-night thermospheric circulation. Heating due to absorption of solar EUV flux, particularly heating due to absorption of solar radiation in the Schumann-Runge continuum region (-130 to 175 nm), is a dominant energy source in the middle and upper thermosphere above —150 km [Killeen, 1987]. The thermospheric heating efficiency of solar ultraviolet photons for varying seasonal and solar cyclical conditions was calculated by Torr et al. [1980a, b] from the data of the <strong>At</strong>mosphere Explorer (AE) satellites. The solar heating rate was estimated from the heating efficiency, and it was used in the thermospheric general circulation models (TGCMs) and other thermospheric
Page 1 and 2: A Study on Middle-scale Variations
Page 3 and 4: Abstract The solar wind energy inje
Page 5 and 6: Contents Acknowledgments Abstract i
Page 7 and 8: 6 Discussions CONTENTS 6.1 Nighttim
Page 9 and 10: x LIST OF FIGURES 2.10 2.11 2.12 2.
Page 11 and 12: xii LIST OF FIGURES 4.8 Fringe prof
Page 13: xiv LIST OF FIGURES 5.23 Same as Fi
Page 17 and 18: 1. INTRODUCTION rate at high latitu
Page 19 and 20: 1. INTRODUCTION 5 Analogous to the
Page 21 and 22: 1. INTRODUCTION 7 thermospheric cir
Page 23 and 24: 1. INTRODUCTION 9 Okano and Kim [19
Page 25 and 26: 1. INTRODUCTION confirmed that the
Page 27 and 28: 1. INTRODUCTION 13 and EUV solar ra
Page 29: 1. INTRODUCTION 15 analytical descr
Page 32 and 33: 18 2. DEVELOPMENT OF THE FABRY-PERO
Page 52 and 53: 38 Er e Z O CE F-F-a Ur) h^-• O 0
Page 54 and 55: i 40 2. DEVELOPMENT OF THE FABRY-PE
Page 56 and 57: 42 2. DEVELOPMENT OF TI E FABRY-PER
Page 58 and 59: 44 2. DEVELOPMENT OF THE FABRY -PER
Page 60 and 61: 46 3. OBSERVATIONS 1) The adjustmen
Page 63: (b) 3. OBSERVATIONS (a) !7lasigum 1
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3. OBSERVATIONS Table 3.1. Summary
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____------- wind velocity line-of-s
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3. OBSERVATIONS 59 All operations o
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Chapter 4 Procedures of Data Anal y
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4. PROCEDURES OF DATA ANALYSIS 63 2
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-, (a) 1000 500 (b) 1000 500 0 0 4.
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as 4. PROCEDURES OF DATA ANALYSIS 6
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wind velocity v is given by 4. PROC
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80 c..1 0 40 ,7u cn 20 0 0 4. PROCE
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,-C btu cu ...-1 7.) al +t) CI a) 1
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o 5000 4. PROCEDURES OF DATA ANALYS
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(a) 800 600 (i) =g-, 400 ›.- Pc C
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80 5. THER.MOSPIIERIC NEUTRAL WINDS
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8 2 5_ THERMOSPHERIC NEUTRAL WINDS
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I E 84 5. TILERMOSPHERIC NEUTRAL WI
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I 05 8 6 5. THERMOSPILERIC NEUTRAL
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88 5. THERMOSPHERIC NEUTRAL WINDS O
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Line-of-Sight Neutral Wind Velociti
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5. THERMOSPIIERIC NEUTRAL WINDS OVE
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0 Cf) CO • imme F.4 Ca) O 7-1)` c
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$.4 RS 4—) 0.0 X.4 P"'"a Pm( tri
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4 0 • U) 4.) O •-4 • -I•ma
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P-1 • p^^4 4.4 • •.* prZ •p
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5. THERMOSPHERIC NEUTRAL WINDS OVER
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Chapter 6 Discussions 6.1 Nighttime
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a_ -1 7 6 5 4 3 2 -2 1 0 - 3 _4 -5
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I = - E ,---, c.) u.) a) ..... c.;
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1 (13 C 7)4 "CI ,;3 C N 0 z 0, 2 Ho
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6. DISCUSSIONS 125 is seen in numer
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6. DISCUSSIONS 6.3 Middle-scale atm
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6. DISCUSSIONS 129 15:50:00 lb:00:0
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132 6. DISCUSSIONS It is very inter
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CAD MAGNE TOGFIRM AT STOWR STA T I
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136 7. CONCLUSIONS 5) Nighttime var
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138 REFERENCES Conde, M., and R. W.
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140 REFERENCES Hernandez, G., R. W.
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142 REFERENCES Rees, D., and A. H.
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Appendix A Sequential wind data in
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Line-of-sight neutral wind velociti
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