- Title Information
- Title
- Water on the Lunar Surface as Seen by the Moon Mineralogy Mapper: Distribution, Abundance, and Origins
- Name:
Personal
- Name Part
- LI, SHUAI
- Role
- Role Term:
Text
- creator
- Origin Information
- Copyright Date
- 2016
- Physical Description
- Extent
- xvi, 295 p.
- digitalOrigin
- born digital
- Note
- Thesis (Ph.D.)--Brown University, 2016
- Name:
Personal
- Name Part
- Milliken, Ralph
- Role
- Role Term:
Text
- Director
- Name:
Personal
- Name Part
- Pieters, Carle
- Role
- Role Term:
Text
- Reader
- Name:
Personal
- Name Part
- Saal, Alberto
- Role
- Role Term:
Text
- Reader
- Name:
Personal
- Name Part
- Head, James
- Role
- Role Term:
Text
- Reader
- Name:
Personal
- Name Part
- Gaddis, Lisa
- Role
- Role Term:
Text
- Reader
- Name:
Corporate
- Name Part
- Brown University. Geological Sciences
- Role
- Role Term:
Text
- sponsor
- Genre (aat)
- theses
- Abstract
- Water is one of the most volatile species in our solar system and cannot condense to solid phase at locations close to the Sun (i.e., < ~3 AU, known as the ‘snow’ line) due to its low condensation temperature [Hayashi, 1981; Podolak and Zucker, 2004; Martin and Livio, 2014]. Yet the water content and distribution on planetary bodies within the ‘snow’ line can provide important constraints on modeling solar system formation and evolution [e.g., Martin and Livio, 2014]. Water on the surface can be assessed with orbital observations, but there is no such technology to assess the hydration state of the interior of a planetary body directly. Alternatively, water associated with internal activities (i.e., magmatism) may provide probes to planetary interiors [Saal et al., 2008]. Our Moon is an ideal place to examine the hydration state both on the surface and in its interior because returned samples and multiple orbital observations are available, although most observations are limited to the surface. The bulk of my research focuses on identifying and quantifying the water (H2O/OH) on the lunar surface and deciphering endogenous and exogenous sources using reflectance spectroscopy and laboratory experiments. Results of this work can provide critical constraints on modeling the formation and evolution of the Earth-Moon system. Additionally, the framework developed in this research can be applied to explore the hydration state at other planetary bodies within the ‘snow’ line of our solar system when similar datasets are available in future, which can provide more data points for improving our understanding on the solar system formation and evolution.
- Subject
- Topic
- Volatiles in the solar system
- Subject
- Topic
- Lunar water
- Subject
- Topic
- Spectroscopy
- Subject
- Topic
- Lunar volcanism
- Record Information
- Record Content Source (marcorg)
- RPB
- Record Creation Date
(encoding="iso8601")
- 20170531
- Identifier:
DOI
- 10.7301/Z09W0CXG
- Access Condition:
rights statement
(href="http://rightsstatements.org/vocab/InC/1.0/")
- In Copyright
- Access Condition:
restriction on access
- Collection is open for research.
- Type of Resource (primo)
- dissertations