Foreword ix Introduction xi Chapter 1. Optical Architecture 1 1.1. Introduction 1 1.2. Optical theories of light phenomena 7 1.3. Optical systems for observation and detection 12 1.
4. Main limitations of an optical system 18 1.4.1. Resolution power and Rayleigh criterion 18 1.4.2. The defects of a real optical instrument 28 1.
4.3. Fourier optics and the spatial frequencies of an object 33 1.5. Light detection system in an optical system 38 1.5.1. Poynting vector and photon detection 39 1.
5.2. Semiconductor-based detectors, photodiodes and CCDs 40 1.6. Application examples 45 1.6.1. Telescope observing the Sun 45 1.
6.2. Spectrometer for measuring the solar spectrum and its variability over time 50 1.7. Conclusion 54 1.8. Appendix 55 1.8.
1. Propagation of light in wave optics 55 1.8.2. Terrestrial radiation sensors 60 Chapter 2. Thermal and Electrical Architectures 65 2.1. Introduction 65 2.
2. Electrical architecture of a CubeSat 69 2.2.1. The various components of electrical architecture 69 2.2.2. The attitude control system 72 2.
3. Thermal architecture of a CubeSat 75 2.3.1. Thermal control 76 2.3.2. Thermal specifications for CubeSats 77 2.
3.3. Thermal management technologies for CubeSats 78 2.4. Development and evaluation of thermal control 84 2.4.1. Phase 0: analysis 85 2.
4.2. Phase A: feasibility study 85 2.4.3. Phase B: preliminary definition 85 2.4.4.
Phases C and D: implementation and qualification 85 2.4.5. Phase E: in-orbit operation and decommissioning 87 2.5. Theories, models and simulation of thermal effects 87 2.5.1.
Heat transfer by conduction, convection and radiation 88 2.5.2. Heat diffusion equation 94 2.5.3. Devices or systems used for thermal effects management 95 2.5.
4. Example of an equation for heat diffusion in a telescope 99 2.6. Conclusion 104 2.7. Appendix 105 2.7.1.
Quantities characterizing the exchange of luminous flux by radiation 105 2.7.2. View factor 109 2.7.3. Thermal environment in space 113 2.7.
4. Theoretical elements relating to thermomechanics and thermoelasticity 115 2.7.5. TRL scale (Technology Readiness Level - ISO 16290-2013) 119 Chapter 3. Environmental Testing 121 3.1. Introduction 121 3.
2. Main limitations of a spatial system 127 3.2.1. The FIDES benchmark for predictive reliability 127 3.2.2. Reliability through RBDO simulation and digital twin procedure 132 3.
3. Constraints of the space environment on the design of space systems 142 3.3.1. Mechanical launch environment 142 3.3.2. Orbital environment 143 3.
3.3. Space environment 143 3.4. Solar cycles 143 3.4.1. Long-term solar cycle index 146 3.
4.2. Short-term solar cycle index 146 3.5. The effects of the gravitational field 147 3.5.1. Gravitational force 147 3.
5.2. Microgravity 147 3.5.3. The atmospheric model, or neutral atmosphere 148 3.5.4.
The gaseous constituents of the atmosphere at high altitude 149 3.5.5. The altitude density model 149 3.5.6. Aerodynamic drag 150 3.6.
The effects of the magnetic field 151 3.6.1. Origin and variation of the geomagnetic field 152 3.6.2. The magnetosphere and its characteristics 152 3.6.
3. The external magnetic field and its characteristics 154 3.6.4. Magnetic field model and nominal values 154 3.6.5. Nominal values and characteristics of the magnetic field 155 3.
6.6. South Atlantic Anomaly (SAA) 155 3.7. Effects due to plasma 156 3.7.1. Plasma environment in low Earth orbit 157 3.
7.2. Plasma temperatures 158 3.7.3. Electrical charging and effects on the satellite 159 3.7.4.
Effects of radiation 159 3.7.5. Effects of the Van Allen belt 161 3.7.6. Electromagnetic radiation 161 3.7.
7. Satellite lifespan 161 3.8. Conclusion 162 3.9. Appendix 163 3.9.1.
Statistics and probabilities, and generalized extremum law 163 3.9.2. Example of thermal effect simulation using FEM 172 3.9.3. Preparation of the CubeSat: UVSQ-SAT NG 179 Chapter 4. Preparing for an Observation Mission 181 4.
1. Introduction 182 4.2. Calibration of the UVSQ-SAT NG NIR spectrometer 186 4.2.1. Wavelength calibration 187 4.2.
2. Absolute response 191 4.2.3. Bandwidth and aperture function 193 4.2.4. Temperature 196 4.
3. Determination of the extraterrestrial solar spectrum using the Langley tracing technique 197 4.3.1. Methodology 198 4.3.2. Considering atmospheric effects 200 4.
3.3. Calculation of optical depth 202 4.3.4. Conditions for accurate measurements using the Langley technique 202 4.4. Experimental results and discussion 203 4.
5. Conclusion 209 4.6. Appendix 210 4.6.1. Analysis and processing of measurement data 210 4.6.
2. The nonlinear simplex method 216 4.6.3. The Levenberg-Marquardt method 219 4.6.4. The Broyden-Fletcher-Goldfarb-Shanno method 221 4.
6.5. Signal processing for deconvolving a measurement 221 4.6.6. Spectrum of a diatomic molecule in IR spectroscopy 226 Chapter 5. A Better Understanding of Light 233 5.1.
The period from Antiquity to the Middle Ages 233 5.2. Initial approaches to interpreting light phenomena 235 5.3. First theorems and postulates of optics 238 5.4. Two teaching methods: Neoplatonism and Scholasticism 240 5.5.
Science in the Middle East 241 5.6. Universities and science in Europe 243 5.7. Optics after the Middle Ages and the scientific revolution 248 5.7.1. The law of refraction and the speed of light in a medium 248 5.
7.2. Geometric optics and wave optics 249 5.7.3. Photons and stimulated emission 250 5.7.4.
Quantum optics and photon entanglement 253 5.8. Conclusion 256 5.9. Appendix 257 5.9.1. Elements of quantum mechanics 257 5.
9.2. Thermal transfer modeling using the density matrix 260 5.9.3. The nature of the photon and the quantum vacuum 265 Conclusion 275 References 277 Index 301.