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iv ABSTRACT largest around midnight. The difference is supposed to be associated with the auroral energy injection and the relative location between the auroral oval and Syowa station. 2) In the vicinity of auroral arcs, strong outward flows were often observed. These flows seem to be caused by forced convection which is the response to heating or the divergent component of ion drag around auroral arcs. However, the velocity of outward flows were much greater than the prediction of numerical models. 3) Periodic enhancements of meridional winds which are classified into middle-scale atmo- spheric gravity waves (AGWs) were observed on the night of 3-4 June 1994 during geomag- netically active periods. The period of the variations was 1.3 — 2 hr and 1.2 hr in the F- and E-region, respectively, while the phase velocity of the poleward propagation was —80 m/s and —110 m/s in the F- and E-region, respectively. These middle-scale AGWs appear to be generated in the auroral oval staying at a few hundred kilometers north of Syowa station. This is the first case that the generation and propagation of middle-scale AGWs were clearly observed by an optical method. 4) Strong divergent wind patterns which suggest the existence of strong upward thermospheric winds were observed three times on the same night of 3-4 June 1994. The events appeared on the poleward side of the auroral oval at 0246 UT and 0302 UT seemed to be similar events reported by Price et al. [1995]. The event which occured at 0404 — 0413 UT on 4 June 1994 showed a dramatic enhancement of the divergent wind which has not been reported yet. The upwelling region and the 01630.0 rim auroral emission region overlapped each other, and the strong divergent wind was generated simultaneously with an auroral emission enhancement. Its duration was —15 min, and the horizontal scale of the upwelling region was estimated to be more than 680 km in the F-region. These observational results demonstrate that the FPDIS is an outstanding tool for re- mote sensing of rapid variations of the thermospheric neutral winds associated with auroral activity, and make clear the existance of several types of thermospheric responses to auroral activity. Furthermore, it is demonstrated that the upwelling motion observed near the active auroral region is closely related with the AGW generation.
Contents Acknowledgments Abstract iii Contents V List List of Figures of Tables 1 Introduction 1.1 The Earth's thermosphere L2 Modeling and simulation of the thermosphere 1.2.1 Thermospheric general circulation models 1.2.2 Empirical models 1.2.3 Other modeling and simulations 1.3 Satellite observations of the thermospheric neutral wind 1.4 Ground-based observations of the high-latitude thermospheric neutral wind 1.4.1 Upper thermosphere 1.4.2 Lower thermosphere 1.4.3 Vertical winds 1.5 Purpose of this thesis 2 Development of the Fabry-Perot Doppler Imaging System 2.1 Basic principle of the Fabry-Perot interferometer 2.2 Principle of the Fabry-Perot Doppler imaging 2.3 Prototype of the Fabry-Perot Doppler Imaging System • viii XV 1 1 3 3 4 5 6 8 8 11 13 14 17 17 19 24
Page 1 and 2: A Study on Middle-scale Variations
Page 3: Abstract The solar wind energy inje
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 and 14: xiv LIST OF FIGURES 5.23 Same as Fi
Page 15 and 16: Chapter 1 Introduction 1.1 The Eart
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
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i 40 2. DEVELOPMENT OF THE FABRY-PE
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42 2. DEVELOPMENT OF TI E FABRY-PER
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44 2. DEVELOPMENT OF THE FABRY -PER
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46 3. OBSERVATIONS 1) The adjustmen
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(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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Page 127:
Page 131 and 132:
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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