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22 2. DEVELOPMENT OF THE FABRY-PEROT DOPPLER IMAGING SYSTEM The principle of the Fabry-Perot Doppler imaging system is as follows. Figure 2.3 shows the basic concept of the Fabry-Perot Doppler imaging system which includes an objective lens, a Fabry-Perot interferometer and an image plane detector. In this geometry, a monochromatic light with a wavelength A from a point P0, which is considered to be a small part of a plane emission surface such as auroral emission, falls upon the objective fish-eye lens with an incident angle 0, and focused on a point P1 at the 1-st aperture. Then, the light falls upon the Fabry-Perot interferometer with an angle 0, and focused at a point P2 on the image plane. The light intensity at P2 has a maximum at the light incident angle 0, which satisfies equation 2.10, and thus interference fringes are produced on the image plane. Since the transmittance of the FPI is symmetrical about the optical axis, the produced interference fringes become ring shaped. These fringes are called ' etalon fringes'. An example of the etalon fringes is shown in Figure 2.4. It is found that each segment on the fringes is mapped to the different location of the emission source in the sky. On the other hand, if n and d are constant in equation 2.10, the incident angle 0 and the corresponding fringe radius are decided by the wavelength A. With this theory, we can estimate a slight change of wavelength such as a Doppler shift of auroral emission by measuring the fringe radius precisely. A region where the order numbers of fringes do not overlap is called a free spectral range' AAR. When an interference fringe of m-th order is formed for an incident angle 0 with an interference condition of equation 2.10, the interference fringe of (m + 1)-th order is formed at the incident angle of 0 — AO, i.e., Ern 1 + —X) 7r A = 2nd cos(0 A0). (2.11) On the other hand, when a light with a wavelength of A + AA forms the interference fringe of m-th order at the same incident angle of 4) AO, the following equation is satisfied. m + (A -4- AA) = 2nd cos(4) — AO). (2.12) 71" From equations 2.10, 2.11 and 2.12, the free spectral range AAR is given by AA A2 R -=- AA = 2nd (2.13) cos(1). If the emission line width of an incident light is wider than the free spectral range AAR, it is difficult to isolate each emission line spectrum, since adjoining fringes with different order numbers overlap each other.
0 2. DEVELOPMENT OF THE FABRY-PEROT DOPPLER IMAGING SYSTEM 23 190 r---$ C (/) a) Figure 2.4. An example of interference fringes of a Fabry-Perot etalon. These are fringes of a lie-Ne laser source with a etalon of 12 mm spacer and a reflectance of 0.88.
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 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
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
Page 67 and 68: 3. OBSERVATIONS Table 3.1. Summary
Page 69: ____------- wind velocity line-of-s
Page 73 and 74: 3. OBSERVATIONS 59 All operations o
Page 75 and 76: Chapter 4 Procedures of Data Anal y
Page 77 and 78: 4. PROCEDURES OF DATA ANALYSIS 63 2
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Page 81 and 82: as 4. PROCEDURES OF DATA ANALYSIS 6
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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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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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