Introduction
- Definition of volatiles
- Old view of volatiles
- Significance of volatiles
- Reservoirs of volatiles
Quantifying Present Day Volatiles
- Abundance
- PSRs—LCROSS, LEND/LPNS, LAMP, LOLA, visible images LROC & Kaguya, radar
- Global—M3/Cassini/EPOXI, LAMP, LOLA, Apollo samples
- Composition
- PSRs—LCROSS
- Global—Apollo samples, M3/Cassini/EPOXI, lab irradiation spectral, exosphere composition
- Distribution
- PSRs lateral distribution—LAMP, LOLA, LEND/LPNS, Mini-RF
- PSRs depth distribution—LEND/LPNS, Mini-RF
- Global latitudinal distribution—LAMP, M3/EPOXI
- Global local time distribution—LAMP, M3/EPOXI
- Other temporal variability
- Physical Form
- PSR Radar data
- PSR LCROSS—ice grains, H2 abundance/timing
- Global 2.8/3.0 um spectral shape
Volatile System
- Sources
- Comets—model impacts and retention; expected flux
- Meteoroids—model impact and retention; LADEE NMS H2O observations; Apollo sample isotopic analysis
- Solar wind—Apollo agglutinates isotopic analysis, H budget from Kaguya H+, ARTEMIS H+, Chandrayaan-1 H, IBEX H, LAMP H2; lab studies of ion irradiation of lunar soils/rocks; swirls
- Outgassing—Aristarchus, He & Ar LADEE NMS data, Schroedinger
- Redistribution
- Migration/hopping in exosphere
- Migration/diffusion through regolith
- Impact gardening
- Stability
- Thermal mapping—Diviner
- Sublimation stability
- Adsorption stability
- Depth to thermally stable zone
- Orbital evolution effects on thermal stability
- Loss
- Sputtering
- Impact vaporization
- Photodesorption/dissociation
- Sublimation/thermal desorption
Outstanding Questions
- Complete quantification of current contents
- Age of deposits
- Replenishing rate
- Relative importance of sources
- Accessibility
- Differences between Moon and Mercury, Asteroids, meteorites