Optics of the Moon

1st Edition - January 16, 2025
Imprint: Elsevier
Authors: Yuriy Shkuratov, Gorden Videen, Vadym Kaydash
Language: English
Paperback ISBN:
9 7 8 - 0 - 1 2 - 8 1 7 9 7 2 - 7
eBook ISBN:
9 7 8 - 0 - 1 2 - 8 1 7 9 7 3 - 4

Optics of the Moon offers a modern approach to lunar remote sensing. It presents methods for interpreting optics of surfaces with complicated structures, in particular, the lu… Read more

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Optics of the Moon offers a modern approach to lunar remote sensing. It presents methods for interpreting optics of surfaces with complicated structures, in particular, the lunar regolith. For example, this book illustrates how phase-ratio techniques can lead to the detection of surface structure anomalies and describes polarimetric studies of the lunar surface and their use. This book addresses many questions related to the surfaces of the Moon, such as why the Moon looks like a ball at a large phase angle and like a disk in full moon, why the lunar surface has slight color variations, and why at large phase angles its polarization degree closely correlates with albedo.

Including historical perspectives, case studies, maps, and figures to enhance the understanding of both theory and techniques, Optics of the Moon is a valuable resource for researchers and students in lunar and planetary science and remote sensing.

Title of Book
Cover image
Title page
Table of Contents
Copyright
About the authors
Preface
Chapter 1. Lunar histories
1.1 Nostalgic retrospect
1.1.1 Cradle
1.1.2 Telescopic inventions and first lunar observations
1.1.3 Visual studies
1.1.4 Photographic observations
1.1.4.1 Basis of classical photography
1.1.4.2 A few historical remarks
1.1.4.3 Applying the photographic method
1.1.5 Photoelectric technique
1.1.5.1 Photoelement/photomultiplier
1.1.5.2 Panoramic detectors
1.1.6 Empirical and simplified modeling
1.1.7 Laboratory modeling
1.2 Lunar prelude
1.2.1 Past and present
1.2.2 Short geological outline
1.2.3 Atmosphere
1.2.3.1 Gas
1.2.3.2 Dust
1.2.4 Space exploration
Chapter 2. Observational lunar photometry
2.1 Basic definitions
2.1.1 Introduction
2.1.2 Angle variables
2.1.3 Initial notions
2.1.4 Two classical photometric functions
2.2 Characterizing reflectance
2.2.1 Earth-based photometry
2.2.2 Normal albedo mapping
2.2.3 Absolute calibration
2.3 Disk function
2.3.1 Global brightness trend
2.3.2 Comparing disk functions
2.3.3 Equator-pole photometric asymmetry of local slopes
2.3.4 Photometric topography
2.3.4.1 Photogrammetry
2.3.4.2 Photoclinometry
2.4 Phase function
2.4.1 Disk-integrated photometry
2.4.2 Disk-resolved photometry
2.5 Opposition effect
2.5.1 Clementine data
2.5.2 LRO NAC data
2.5.3 Earth-based observations
2.6 Phase functions of color-ratios
2.6.1 Ground-based observations
2.6.2 Laboratory measurements
2.6.3 Measurements from Chandrayaan 1
Chapter 3. Phase-ratio imaging of the Moon
3.1 Introduction
3.2 Earth-based observations
3.2.1 Scales of full disk
3.2.2 Photometric anomalies
3.3 Examples of LRO data applications
3.3.1 Anomaly in Mare Nubium
3.3.2 Reiner Gamma formation
3.4 Fresh craters
3.4.1 Home-made bombardments
3.4.2 Meteoroid impacts
3.5 Giordano Bruno
3.5.1 Headnote
3.5.2 Parameter of optical roughness
3.5.3 Discussion
3.6 Collapsing structures
3.6.1 Ina formation
3.6.2 Lunar fishing
3.7 Apollo missions
3.7.1 Headnote
3.7.2 Apollo 11
3.7.3 Apollo 12
3.7.4 Apollo 14
3.7.5 Apollo 15
3.7.6 Apollo 16
3.7.7 Apollo 17
3.8 Soviet landing probes
3.8.1 Short history
3.8.2 Lunokhod 1
3.8.3 Luna 16
3.8.4 Luna 20
3.8.5 Luna 23
3.8.6 Luna 24
3.8.7 Dust blowing by engine jets
Chapter 4. Elementary basis of lunar spectroscopy
4.1 An overview of spectral mechanisms
4.1.1 Headnote
4.1.2 Radio-wave and infrared reflectance
4.1.2.1 Radio-wave range
4.1.2.2 Infrared range
4.1.3 Visual, NIR, and UV ranges
4.1.3.1 Electronic bands
4.1.3.2 Interaction with UV radiation
4.1.3.3 Influence of lattice defects
4.1.3.4 Nano-phase metallic iron
4.1.3.5 Impurities of rust
4.1.3.6 Solar-wind iron
4.2 A few spectral mechanisms in more detail
4.2.1 Simple model of fundamental absorption bands
4.2.1.1 Oscillator model
4.2.1.2 Mixing formulae
4.2.2 Elements of ligand-field theory
4.2.2.1 Hydrogen-like atoms
4.2.2.2 Crystal-field bands
4.2.2.3 Charge-transfer bands
4.2.3 Applying the ligand model
4.2.3.1 Pyroxenes
4.2.3.2 Olivines
4.2.3.3 Plagioclases
4.2.3.4 Ilmenite
4.2.3.5 Lunar jewelry (spinels)
4.2.3.6 Glasses
4.2.4 Interaction with hard radiation
4.2.4.1 X-ray spectroscopy
4.2.4.2 Gamma-ray spectrometry
4.3 Scattering in particulate surfaces
4.3.1 A ray-tracing 3D model
4.3.2 An analytical 1D model
4.3.3 1D-model applications
4.3.3.1 Dependence on model parameters
4.3.3.2 Powder mixtures
4.3.3.3 Why does TiO2 correlate with the color ratio?
Chapter 5. Imaging the Moon's spectral parameters: Chemical and mineral composition
5.1 Chemical composition mapping
5.1.1 Simple approaches as applied to ground-based observations
5.1.2 Separation of composition and maturity degree
5.1.3 Several exotic formations revisited
5.1.3.1 Collapsing structures
5.1.3.2 Reiner Gamma
5.1.4 Approach based on LSСС data
5.1.4.1 OMAT, maturity degree, and agglutinate abundance
5.1.4.2 FeO in agglutinates
5.1.4.3 Particle size assessment
5.1.5 A few maps that should not be forgotten in the bustle
5.1.5.1 Imaging what should not be imaged with optical methods
5.1.5.2 Applications of Artificial Neural Networks
5.1.5.3 Clark-Lucey approach as applied to Mg# mapping
5.1.5.4 Mapping of 3He abundance
5.2 Imaging mineral content
5.2.1 Clark-Lucey approach as applied to mineral mapping
5.2.2 Using LSCC data
5.2.3 Chandrayaan 1 M3 data
5.2.3.1 Preamble
5.2.3.2 Data improvement
5.2.3.3 Parameters of the 1 and 2 μm bands
5.2.3.4 Ilmenite mapping
5.2.3.5 Spinel mapping
Chapter 6. Thermal radiation and other tools to study hydrogen compounds of the lunar surface
6.1 Emission radiation
6.1.1 Introduction
6.1.2 A few applications of Kirchhoff's law and Planck's formula
6.1.2.1 Kirchhoff's law and IR imaging
6.1.2.2 Maximal surface temperature
6.1.2.3 Betwixt emission and reflection
6.1.2.4 Two unusual temperature effects
6.1.3 Solid surface temperature
6.1.3.1 Introduction
6.1.3.2 Approximate but pragmatic solution
6.1.3.3 Comparison of measurements and computations
6.1.3.4 Mapping of thermal inertia
6.2 Would you like some water?
6.2.1 What is water?
6.2.2 A few historical remarks
6.2.3 Attempts of radar detection
6.2.4 Neutron spectroscopy
6.2.5 LCROSS cross
6.2.6 MIP sweep
6.2.7 LAMP trump
6.2.8 Using overtone and combination modes
6.3 IR-spectroscopy of H2O/OH– compounds
6.3.1 Band near 3μm
6.3.2 Removal of emission component
6.3.3 Some effects of anisothermality
6.3.3.1 Resolved-topography anisothermality
6.3.3.2 Unresolved-topography anisothermality
6.3.4 Band near 6.1μm
6.4 Mechanisms of H2O/OH– compounds formation
6.4.1 Interior origin of H2O/OH– and other volatiles
6.4.2 Water delivery from comets and meteoroids in late epochs
6.4.3 Superficial hydrogen compounds caused by the solar wind
6.4.4 Time variations of 3μm band
Chapter 7. Lunar polarimetry: Observations with telescopes as well as laboratory, computer, and theoretical modelings
7.1 Parameters
7.2 Telescopic observations
7.2.1 Negative branch
7.2.1.1 Discrete measurements
7.2.1.2 Imaging
7.2.2 Positive branch
7.2.2.1 Discrete measurements
7.2.2.2 Imaging
7.2.2.3 Polarimetric color-ratios
7.2.2.4 Explaining polarimetric color ratios
7.2.2.5 Polarimetric phase ratios
7.2.3 Other polarimetric measurements
7.2.3.1 Orientation of polarization plane
7.2.3.2 Circular polarization
7.2.3.3 Depolarization
7.2.3.4 First spaceborne polarimetry
7.3 Laboratory simulations
7.3.1 Small phase angles
7.3.1.1 Rock or powder?
7.3.1.2 Particle size
7.3.1.3 Surface porosity
7.3.1.4 Albedo
7.3.1.5 Surface tilts and anisotropic topography
7.3.1.6 Surface heterogeneity
7.3.1.7 Interparticle or independent particle scattering?
7.3.2 Large phase angles
7.3.2.1 Particle size
7.3.2.2 Volume density and microtopography
7.3.2.3 Correlation of Pmax with albedo
7.4 Computer modeling and theorizing
7.4.1 Ray-tracing modeling
7.4.2 Ray-tracing with interference of trajectories
7.4.3 DDA approximation
7.4.4 Two rigorous results important for approximations
7.4.4.1 Surprise from T-matrix computations
7.4.4.2 DGTD solution
7.4.5 Practical approaches
7.4.5.1 Empirical formulae
7.4.5.2 Is there a rigorous theoretical standard?
7.4.5.3 Single and double scattering
7.4.5.4 Approximate but simple
Chapter 8. Advanced theorizing and modeling in lunar photometry
8.1 Introduction
8.2 Single-particle scattering
8.2.1 Small particles
8.2.2 Large particles
8.2.3 Single scattering in the H-model
8.3 Shadowing on random topography
8.3.1 H-model
8.3.2 Two-point approximation
8.3.3 Numerical simulation of topography shadowing
8.3.4 Cold traps
8.4 Shadowing effect in particulate media
8.4.1 Light heuristic model
8.4.2 Model of intersected cylinders
8.4.3 Model of two-point correlation
8.5 Multiple scattering in particulate media
8.5.1 Simplest approach
8.5.2 Nonisotropic phase function of particles
8.5.3 Computer experiments with particulate media
8.5.3.1 Describing the method
8.5.3.2 Comparison with radiative-transfer theory
8.5.3.3 Different particulate media
8.5.3.4 Hierarchically arranged structures
8.6 Coherent-backscattering enhancement
8.6.1 Heuristic approach
8.6.2 More rigorous considerations
8.7 Sophisticated model
8.8 Photometric functions for gourmets
8.8.1 Introduction
8.8.2 Equation and general solution
8.8.3 Initial conditions
8.8.3.1 Lambertian law
8.8.3.2 Minnaert law
8.8.4 Playing with parameters
8.8.5 Applications
Index

Yuriy Shkuratov

Professor Yuriy Shkuratov is Department Head for the Astronomy Department at V.N. Karazin Kharkiv National University. He was also the Director of the Astronomical Institute of V.N. Karazin Kharkiv National University from 2004-2014. He is also Leading Research Scientist of Radio Astronomy Institute of the National Academy of Sciences of Ukraine. He has more than 700 scientific publications devoted to the investigation of optical properties of solid surfaces of celestial bodies and arbitrary shaped particles. These works include chapters for seven collective monographs. He first obtained images of polarimetric anomalies of the Moon at large phase angles. He has performed numerous laboratory photometric and polarimetric measurements of structure analogs of the lunar regolith, which provide a reliable experimental basis for the verification and selection of theoretical models for the opposition effect and negative polarization. He has contributed theoretical models of light scattering by particles and surfaces with complicated structure. In particular, he first proposed the model of negative polarization based on the mechanism of coherent backscatter enhancement.

Affiliations and expertise

Professor and Astronomy Dept. Head, V.N. Karazin Kharkiv National University, Ukraine

Gorden Videen

Dr. Gorden Videen is a research scientist at the Space Science Institute and adjunct faculty member at Texas A&M University. He also has worked on optical characterization of aerosols for the Army Research Laboratory and worked as a Program Manager in Atmospheric Science at the Army Research Office. He has been a Visiting Scientist at the University of Amsterdam, Univerisdad de Cantabria and Kyung Hee University. His background is in optics and he has performed experimental, theoretical, and modeling work investigating polarimetric light scattering and remote sensing of complex systems ranging from atmospheric aerosols and cometary comae to extended regolith systems. Many of these works have focused on obtaining information from the polarization and light-scattering properties of the systems, including the lunar regolith.

Affiliations and expertise

Senior Research Scientist, Space Science Institute, US

Vadym Kaydash

Dr. Vadym Kaydash is Senior Research Scientist and the Director of the Astronomical Institute of V.N. Karazin Kharkiv National University. His research includes analysis and interpretation of Hubble Space Telescope imaging polarimetry of aerosols of the Martian atmosphere, photometric anomalies of the lunar surface using data of SMART-1 lunar mission, and mapping the photometric function variations and the polarization parameters for the nearside of the Moon by telescopic data.

Affiliations and expertise

Director, Astronomical Institute of V.N. Karazin Kharkiv National University, Ukraine

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Optics of the Moon

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