i Detection of Smoke and Dust Aerosols Using Multi-sensor Satellite ...

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3.1 MODIS Instrument MODIS, one of key sensors of the National Aeronautics and Space Administration (NASA) Earth Observing System (EOS), was launched onboard the Terra spacecraft on December 18, 1999 and the Aqua spacecraft on May 4, 2002 (Barnes et al., 2002; Salomonson et al., 2002). Both Terra and Aqua MODIS are operated in a sun-synchronous orbit at the altitude of 705 km. Terra descends southwards with the local equatorial crossing time 10:30 a.m. and Aqua ascends northwards with the local equatorial crossing time 1:30 p.m. respectively. The MODIS has been widely used for the study of land, ocean, atmosphere, and solid earth etc. (Justice et al., 1998; Esaias et al., 1998; King et al., 2003; Parkinson, 2003). 3.1.1 MODIS spectral band The MODIS makes the Earth observations with 36 bands, covering the wavelength range from 0.4 to 14.2 μm. The 20 RSBs and 16 TEBs are arranged in four FPAs: VIS, NIR, Short- and Middle- Wavelength Infrared (SMIR), and Long- Wavelength Infrared (LWIR), shown in Fig. 3.1 (Che et al., 2005). Three different spatial resolutions are designed according to the band specifications and science applications: 250 m (band 1-2), 500 m (band 3-7), and 1 km (band 8-36). The number of detectors of each band is 40, 20, and 10 respectively corresponding to its spatial resolution (Barnes et al., 2002; Salomonson et al., 2002). The specifications of all spectral bands are listed in Table 3.1. Among these bands, band 1 (red), band 4 (green), and band 3 (blue) are usually used for constructing RGB true color image. The MODIS is a cross-track scanning radiometer 17
with a two-side scan mirror which rotates over a scan angle range of ±55 o , producing a swath of 2330 km in scan direction and 10 km in track direction each scan (Xiong et al., 2007). Figure 3.1: The layout of the MODIS FPAs. All 36 MODIS bands are separated into four FPAs: VIS, NIR, SMIR, and LWIR. The number of detectors of each band varies with the spatial resolution: 40 detectors for 250 m bands, 20 detectors for 500 m bands, and 10 detectors for 1 km bands (Source: Che et al., 2005). 18
Page 1 and 2: Detection of Smoke and Dust Aerosol
Page 3 and 4: DEDICATION This is dedicated to my
Page 5 and 6: TABLE OF CONTENTS Page LIST OF TABL
Page 7 and 8: LIST OF TABLES Table Page Table 1.1
Page 9 and 10: Figure 6.2 The UVAI images and the
Page 11 and 12: VFM Vertical Feature Mask VIS Visib
Page 13 and 14: are validated not only visually wit
Page 15 and 16: 1.1 Importance of Studying Smoke an
Page 17 and 18: 1.3 Objectives and Scopes The main
Page 19 and 20: originalities, and discussions of f
Page 21 and 22: 1.6 Principal Results The principle
Page 23 and 24: CHAPTER 2 REVIEW OF APPROACHES FOR
Page 25 and 26: cooperatively: the reflectance at 0
Page 27 and 28: more information about dust charact
Page 29: CHAPTER 3 SMOKE AEROSOL DETECTION W
Page 33 and 34: 3.1.2 MODIS data The 55 0 scan angl
Page 35 and 36: Sun Satellite Figure 3.2: Basic rad
Page 37 and 38: 1 0 /2 b ( 0 0, 0; , ) k1 e
Page 39 and 40: 3.2.3 Training data collection Surf
Page 41 and 42: Reflectance Reflectance Response cu
Page 43 and 44: Figure 3.6: The normalized ratio of
Page 45 and 46: all pixels over both land and ocean
Page 47 and 48: NDDI 1 0.8 0.6 0.4 0.2 0 -0.2 Figur
Page 49 and 50: MODIS L1B measurements Pixels over
Page 51 and 52: is clear that most of smoke plumes
Page 53 and 54: a b c b Figure 3.10: Smoke images o
Page 55: 3.4.2 California 2007 fire The 2007
Page 58 and 59: The multi-spectral approach is test
Page 60 and 61: 4.1 Physical Principle of Dust Aero
Page 62 and 63: Aqua 2006 102-04/12 04:15 Terra 200
Page 64 and 65: The dust has a high reflectivity at
Page 66 and 67: 0.55 0.5 0.45 0.4 0.35 0.3 0.25 0.2
Page 68 and 69: 7 a Dust pixel 0.5 b 6 Cloud pixel
Page 70 and 71: 4.3 Results Three dust events occur
Page 72 and 73: c c Figure 4.6: Dust storm over TAK
Page 74: 4.4 Chapter Summary In this chapter
Page 77 and 78: operated in the A-train orbit with
Page 79 and 80: 5.1.2 CALIPSO measurements and VFM
Page 81 and 82:
Altitude (km) 20 15 10 5 UTC: 2006-
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After spatial registration, the ove
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Figure 5.4(a) The MODIS true color
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Altitude (km) BTD (K) 20 15 10 15 4
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in the same A-train orbit with simi
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Aqua spacecrafts are operated in th
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the Fig. 6.1a. For easy comparison,
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esolutions, the number of smoke pix
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6.1.4 Validation of dust monitoring
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Figure 6.3 Validation of dust image
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eflectance in red band. Therefore,
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Altitude (km) 20 15 10 5 UTC: 2006-
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image at the same location. The rea
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accuracy could be increased further
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FPAs and cold FPAs (because of diff
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development of future remote sensin
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Figure 7.3: SRCA spatial mode retic
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7.1.3.2 Date Source MODIS L1B data
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characterization. Only the measurem
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these bands, including reflective s
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different spectral bands are slight
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SZA (Degree) SZA (Degree) 65 60 55
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7.2.1.2 Real Impact on L1B Measurem
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7.2.2.1 Theoretical impact analysis
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spatial characterization, the bigge
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Difference NDDI with spatial correc
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8.1 Conclusions CHAPTER 8 CONCLUSIO
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Based on the detection results, the
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3) Validating aerosol detection qua
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REFERENCES Ackerman, S. A., 1989, U
Page 141 and 142:
imagery, Atmospheric Environment, v
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Salomonson, V. V., Privette, J. L.,
Page 145 and 146:
Martinez, A., and Gros, G., 2007-10
Page 147 and 148:
Wang W., Qu, J. J., Liu, Y., Hao, X
Page 149:
CURRICULUM VITAE Yong Xie is a Ph.D
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