Planetary Sciences Community Meetings Calendar
Organized by LPI/USRA *
Results 1 - 50 of 235 found.
January 5-8, 1970
Apollo 11 Lunar Science Conference
(LSC 1970) *,
Houston, Texas
January 11-14, 1971
Second Lunar Science Conference
(LSC 1971) *,
Houston, Texas
January 10-13, 1972
Third Lunar Science Conference
(LSC 1972) *,
Houston, Texas
March 5-8, 1973
Fourth Lunar Science Conference
(LSC 1973) *,
Houston, Texas
March 18-22, 1974
Fifth Lunar Science Conference
(LSC 1974) *,
Houston, Texas
March 17-21, 1975
Sixth Lunar Science Conference
(LSC 1975) *,
Houston, Texas
March 15-19, 1976
Seventh Lunar Science Conference
(LSC 1976) *,
Houston, Texas
March 14-18, 1977
Eighth Lunar Science Conference
(LSC 1977) *,
Houston, Texas
March 13-17, 1978
Ninth Lunar and Planetary Science Conference
(LPSC 1978) *,
Houston, Texas
March 19-23, 1979
Tenth Lunar and Planetary Science Conference
(LPSC 1979) *,
Houston, Texas
March 17-21, 1980
Eleventh Lunar and Planetary Science Conference
(LPSC 1980) *,
Houston, Texas
March 16-20, 1981
Twelfth Lunar and Planetary Science Conference
(LPSC 1981) *,
Houston, Texas
March 15-19, 1982
Thirteenth Lunar and Planetary Science Conference
(LPSC 1982) *,
Houston, Texas
March 14-18, 1983
Fourteenth Lunar and Planetary Science Conference
(LPSC 1983) *,
Houston, Texas
March 12-16, 1984
Fifteenth Lunar and Planetary Science Conference
(LPSC 1984) *,
Houston, Texas
March 11-15, 1985
Sixteenth Lunar and Planetary Science Conference
(LPSC 1985) *,
Houston, Texas
March 17-21, 1986
Seventeenth Lunar and Planetary Science Conference
(LPSC 1986) *,
Houston, Texas
March 16-20, 1987
Eighteenth Lunar and Planetary Science Conference
(LPSC 1987) *,
Houston, Texas
March 14-18, 1988
Ninteenth Lunar and Planetary Science Conference
(LPSC 1988) *,
Houston, Texas
November 14-16, 1988
Workshop on Moon In Transition: Apollo 14, KREEP, and Evolved Lunar Rocks *,
Houston, Texas
March 13-17, 1989
Twentieth Lunar and Planetary Science Conference
(LPSC 1989) *,
Houston, Texas
October 10-11, 1989
Workshop on Lunar Volcanic Glasses: Scientific and Resource Potential *,
Houston, Texas
March 12-16, 1990
21st Lunar and Planetary Science Conference
(LPSC 1990) *,
Houston, Texas
March 18-22, 1991
22st Lunar and Planetary Science Conference
(LPSC 1991) *,
Houston, Texas
March 16-20, 1992
23st Lunar and Planetary Science Conference
(LPSC 1992) *,
Houston, Texas
March 15-19, 1993
24st Lunar and Planetary Science Conference
(LPSC 1993) *,
Houston, Texas
March 14-18, 1994
25st Lunar and Planetary Science Conference
(LPSC 1994) *,
Houston, Texas
November 13-16, 1994
International Lunar Exploration Conference,
San Diego, California
March 13-17, 1995
26th Lunar and Planetary Science Conference
(LPSC 95) *,
Houston, Texas
March 18-22, 1996
27th Lunar and Planetary Science Conference
(LPSC 96) *,
Houston, Texas
March 17-21, 1997
28th Lunar and Planetary Science Conference
(LPSC 97) *,
Houston, Texas
January 9, 1998
Goblins in the Moon: The Moderately Siderophile But Excessively Significant Elements Nickel and Cobalt as Tracers of Lunar History (Graham Ryder, Lunar and Planetary Institute),
Lecture Hall
March 13, 1998
Clementine Imaging of Impact Basins, Probes Into the Lunar Crust (Ben Bussey, European Space Agency)
March 16-20, 1998
29th Lunar and Planetary Science Conference
(LPSC 98) *,
Houston, Texas
March 15-19, 1999
30th Lunar and Planetary Science Conference
(LPSC 99) *,
Houston, Texas
April 2, 1999
The Deep Structure of Lunar Impact Basins (Walter Kiefer, Lunar and Planetary Institute)
July 15-16, 1999
Lunar Base Development Symposium,
League City, Texas
February 8, 2000
The Moon and the Future of NASA (Dr. Paul Spudis, Lunar and Planetary Institute),
Hess Room - Brown Bag Seminar
Contrary to what many believe, NASA has no long-term goal or plan and no process by which such a plan might be developed. The agency has largely been in a "holding pattern" since the lunar landings over 30 years ago, with an Apollo-style management and operational idiom and a NACA-level budget. Although much of the current PR focuses on missions to Mars as the next big program, I suggest instead that the goal of a lunar outpost more readily fits economic, political, and technical realities. Such a program would both create the infrastructure that would allow us to go on to the planets and accomplish significant and recognizable near-term milestones.
March 13-17, 2000
31st Lunar and Planetary Science Conference
(LPSC 2000) *,
Houston, Texas
June 30, 2000
Lunar atmosphere -- Much ado about (next to) nothing (Drew Potter, LPI),
Lecture Hall
September 22, 2000
The Impact Environment During the Origin and Early Evolution of Life on Earth: What the Moon Really Shows (Graham Ryder, Lunar and Planetary Institute),
Lecture Hall
Theoretical studies of the impact environment prior to ~ 3.85 Ga tend to conclude that the Earth suffered repeated potentially sterilizing impact events, and that life could have originated - and then been annihilated - several or numerous times. The impact fluxes used are scaled from a crater density-time curve for lunar history that in fact is not constrained at times before 3.9 Ga. Mass accretion is better constrained, and demonstrates that at least the Nectarian-Early Imbrian time is anomalous in its high accretion rate. Sterilizing-scale impacts on Earth probably did not occur after ~ 4.3 Ga. The origin of life occurred in a comparatively quiescent impact environment.
March 12-16, 2001
32nd Lunar and Planetary Science Conference
(LPSC 2001) *,
Houston, Texas
September 17-19, 2001
New Views of the Moon, Europe: Future Lunar Exploration, Science Objectives, and Integration of Datasets,
Berlin, Germany
September 21, 2001
Lunar Exploration and Mars Exploration - Simularities and Differences (Donald A. Beattie, Consultant and Author ("Taking Science to the Moon")),
Berkner Room
Unmanned lunar exploration programs were conceived in the late 1950s. Although the Ranger and Surveyor programs were started prior to the announcement of Apollo, they soon succumbed to the need to support Apollo. They were reduced in scope, both in types of experiments and number of flights to save money, and reconfigured to provide the early information required to give confidence for the designs of Apollo hardware on the drawing boards. Lunar Orbiter, although proposed at a later date, also was modified and became primarily an Apollo support program. However, the photographic coverage was expanded on the last two missions to include potential post-Apollo landing sites and the final mission was designed to cover as much as possible of the still poorly photographed parts of the Moon, including the backside. Soviet unmanned missions during this timeframe added information and eventually a small amount of sample was returned. The more recent Clementine and Lunar Prospector spacecraft have added new information, however, they were not launched as part of an ongoing, comprehensive plan of lunar exploration.
Apollo, at its inception, had very modest scientific objectives. Collect a few samples, perhaps take some photographs and deploy some experiments (with emphasis on "perhaps"), and complete President Kennedy's mandate without losing any astronauts in a risky venture. By 1964 this view had changed and, little by little, our ability to conduct exploration greatly expanded culminating with the final three "J" missions.
Mars exploration has had a much different evolution. Beginning with the Mariner and Viking missions, unmanned exploration has taken a much more careful and complete evolutionary approach than the unmanned missions that led up to the first Apollo landings. In addition to those already completed or underway, a continuing suite of missions had been proposed by NASA and only time will tell if they will be successfully carried out. Unmanned Mars missions that include small rovers and sample return may resolve the major reason to conduct costly Mars exploration, the unequivocal discovery of life forms. If found, one might ask, is it necessary to continue to explore the red planet? If life forms are not found in returned Mars samples, or for whatever reason samples cannot be returned, then the need, in the minds of some, to continue Mars exploration will still exist.
As we look to the future of Mars exploration, what may be the drivers? A political imperative such as shaped lunar exploration will probably not be established. Human exploration, setting foot on Mars surface just to understand its history and evolution (comparative planetology), will be a hard sell under any circumstances because of cost. Colonization is still science fiction. But what if the search for life becomes a compelling reason and the case is made that only humans on the ground can assure that an answer will be found? Should we prepare for such an eventuality, and if so, what further groundwork needs to be done and how can we apply the lessons from Apollo to help assure success?
March 11-15, 2002
33rd Lunar and Planetary Science Conference
(LPSC 2002) *,
Houston, Texas
August 23, 2002
Space Weathering on Surfaces of Planets, Satellites, and Asteroids (Bruce Hapke, University of Pittsburg),
Berkner Room
The vapor deposition model of space weathering will be discussed. The changes in the optical properties of regoliths of silicate bodies without atmospheres, including spectral darkening, reddening and obscuration of absorption bands, are due to submicroscopic metallic iron, and not impact-vitrified glass, as commonly assumed. The iron particles are created during the deposition of vapor generated by both solar wind sputtering and meteorite impact vaporization. The history of the model will be briefly reviewed. It will be shown to be able to account quantitatively for changes in lunar optical properties, and to predict the alteration of spectra of ordinary chondrites to more closely resemble those of S-asteroids. Applied to Mercury, it implies that this body has a regolith in which FeO is low (~2-6%), but not completely absent.
September 12-14, 2002
The Moon Beyond 2002: Next Steps in Lunar Science and Exploration *,
Taos, New Mexico
November 8, 2002
What We've Learned About the Moon from Lunar Meteorites." (Dr. Randy Korotev, Washington University, St. Louis),
Berkner Room
About two dozen meteorites from the Moon have been recognized in the past 20 years. Despite the fact that we have 382 kg of lunar samples from 6 Apollo and 3 Russian Luna missions, the lunar meteorites are providing some important new insights about the geology and geochemistry of the Moon. Although random samples from the lunar surface, they provide a type of ground truth for orbiting remote-sensing missions.
March 17-21, 2003
34th Lunar and Planetary Science Conference
(LPSC 2003) *,
Houston, Texas
November 12, 2003
Turning Rock Into Regolith - Space Weathering in the Inner Solar System (Sarah Noble, Brown University),
Hess Room - Brown Bag Seminar
Any body that does not have an atmosphere to protect it should suffer the effects of space weathering, however those processes are dependent on their environment (e.g. soil composition, bombardment rate and velocity, distance from the sun, strength of gravity, temperature, existence of a magnetic field, etc.), and thus should vary from body to body. "Space weathering" may therefore look different on Mercury or the asteroids than it does on the Moon. It appears, for example, that the extreme temperature range on Mercury may have significant consequences for the properties of space weathering there. As for the asteroids, as we have no direct regolith samples from these bodies with which to compare to our lunar samples, we have been comparing and contrasting lunar regolith breccia samples to meteoritic regolith breccias in order to try to understand regolith processes on asteroids. In addition, we have created a synthetic optical analog for space weathering products that allows us to investigate how the optical properties of space weathered material changes under different conditions. By revealing the differences in weathering effects distance from the sun, strength of gravity, temperature, existence of a magnetic field, etc.), and thus should vary from body to body. "Space weathering" may therefore look different on Mercury or the asteroids than it does on the Moon. It appears, for example, that the extreme temperature range on Mercury may have significant consequences for the properties of space weathering there. As for the asteroids, as we have no direct regolith samples from these bodies with which to compare to our lunar samples, we have been comparing and contrasting lunar regolith breccia samples to meteoritic regolith breccias in order to try to understand regolith processes on asteroids. In addition, we have created a synthetic optical analog for space weathering products that allows us to investigate how the optical properties of space weathered material changes under different conditions. By revealing the differences in weathering effects distance from the sun, strength of gravity, temperature, existence of a magnetic field, etc.), and thus should vary from body to body. "Space weathering" may therefore look different on Mercury or the asteroids than it does on the Moon. It appears, for example, that the extreme temperature range on Mercury may have significant consequences for the properties of space weathering there. As for the asteroids, as we have no direct regolith samples from these bodies with which to compare to our lunar samples, we have been comparing and contrasting lunar regolith breccia samples to meteoritic regolith breccias in order to try to understand regolith processes on asteroids. In addition, we have created a synthetic optical analog for space weathering products that allows us to investigate how the optical properties of space weathered material changes under different conditions. By revealing the differences in weathering effects with different environments and compositions, we can begin to understand the fundamental processes of space weathering and the relative importance of the many external and internal factors involved. This knowledge will allow us to make more accurate predictions about the effects of exposure to the space environment on bodies from which we have no samples, which in turn will allow us to more accurately interpret remotely sensed data of those bodies.