Sequestration of organic matter (OM) in sediments is a fundamental
biogeochemical process, regulating atmospheric CO2 and O2 cycling among
many other processes. The controls on OM sequestration are remarkably
contentious. Studies of geological OM deposits have stressed the dominance
of oceanographic controls such as bottom water anoxia or upwelling-induced
productivity. Independently, a paradigm of mineral surface area (MSA)
control of OM sequestration has developed in soil science and studies of
modern marine sediments. This mechanism has rarely been considered for
ancient organic-rich sediments, though these sediments are commonly used to
infer past oceanographic conditions.

Widespread intervals of organic rich deposits evident in the geologic
record are topical because they help to form our view of the Earth system
at critical warm intervals in its past history, and thus provide insight in
to potential ocean conditions with future warming. Should mineral surfaces
be as important to carbon burial in the past as they appear to be in the
modern, then it is possible that some successions of organic rich rocks
tell a very different story, one in which continental climate variation can
regulate long term carbon deposition. Further, because clay minerals that
control MSA form in equilibrium with ambient continental climates, an
MSA:TOC relation implies a feedback between changes in continental climate
and carbon burial not previously recognized. In this talk I will present
data showing an increase in clay mineral deposition in marine sediments
coinciding with, and likely responsible for enhanced carbon burial and a
critical rise in oxygen at the end of the Precambrian facilitating animal
evolution. I will also show studies of Cretaceous continental margin
sediments identifying potential future patterns of carbon burial and a
strong negative feedback active in greenhouse conditions.

Enceladus, a moon of Saturn 500 km in diameter, spews out a mixture of
water vapor and other gases, ice particles with dissolved salts, and
infrared radiation that implies a warm interior. "How warm" is the big
question, and liquid water is the answer everyone is wondering about. I
will first review the observations, most of which come from instruments
aboard Cassini. Then I will present the results of a hydrodynamic model of
an ice/vapor mixture (Ingersoll and Pankine, Icarus, in press). The model
gives the properties of the mixture as it leaves the icy conduit. If no
liquid is present, the ice particles must condense from the vapor, but the
ice/vapor ratio is less than 2%. Then I present an analysis of Cassini
imaging data that points to ice/vapor ratios approaching 50% (Ingersoll and
Ewald, Icarus, submitted). The implication is that the source for the
plumes is a boiling liquid rather than a condensing vapor. Enceladus has
passed a few tests of "habitability," but we are still a long way from
saying that it is inhabited.

On June 18, 2009, NASA launched the Lunar Reconnaissance Orbiter (LRO) and
the Lunar Crater Observation and Sensing Satellite (LCROSS) spacecraft. One
of the main goals of both missions is to search for evidence of ice at the
lunar poles. LRO has now acquired extensive mapping data at the lunar poles
and LCROSS has successfully impacted a permanently shadowed crater in the
south polar region. From the  initial results of the two missions is
emerging a new picture of the  composition, distribution and history of
lunar polar volatiles. The talk  will focus on the results of the LRO
Diviner Lunar Radiometer Experiment  which has acquired extensive polar
mapping data, as well as direct  observations of the LCROSS impact.

Prof. Paige specializes in surfaces, ice caps, atmospheres, and climates
of terrestrial planets, using both remote sensing and lander methods. He
has studied (potential) polar ices on Mars, the Moon, Mercury, Pluto, and
Triton.

Cassini-renewed exploration of Titan's high southern latitudes by  
RADAR has revealed changes in major lacustrine features, as well as  
extensive fluvial networks that suggest periods of methane and  
possibly ethane flow. The results further emphasize Titan as a place  
where seasonal cycling as well as longer term climate cycles are in  
play. Finally, I will discuss the larger context of Titan's climate,  
as a model for the climate of Earth in the far future, and as an  
exemplar of planets in stable, quasi-1AU environments around the most  
common type of star in the cosmos.

ESS should attend Wednesday AOS/ESS talk by Andy Ingersoll on MJO