Saturday, February 6, 2016
Edgar Mitchell (1930-2016)
Tuesday, November 19, 2013
Lunar Laser Ranging: The Millimeter Challenge
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| The five Lunar Laser Range Reflector (LLR or LLRR) arrays deployed on the lunar surface, one each at the landing sites of Apollo 11, 14 and 15, and also to the Soviet rovers Lunokhod 1 and 2. The sublime accuracy of the decades-long measurements are priceless to astrophysics. Nearside view from "Synthetic View of the Moon," LROC Featured Image released October 15, 2013 [NASA/GSFC/Arizona State University]. |
Center for Astrophysics and Space Sciences
University of California
Lunar laser ranging has provided many of the best tests of gravitation since the first Apollo astronauts landed on the Moon. The march to higher precision continues to this day, now entering the millimeter regime and promising continued improvement in scientific results. This review introduces key aspects of the technique, details the motivations, observables, and results for a variety of science objectives, summarizes the current state of the art, highlights new developments in the field, describes the modeling challenges and looks to the future of the enterprise.
Since 1969, lunar laser ranging (LLR) has provided high-precision measurements of the Earth-Moon distance, contributing to the foundations of our knowledge in gravitation and planetary physics. While being the most evident force of nature, gravity is in fact the weakest of the fundamental forces, and consequently the most poorly tested by modern experiments. Einstein's general relativity, currently our best description of gravity, is fundamentally incompatible with quantum mechanics and is likely to be replaced by a more complete theory in the future. A modified theory would, for example, predict small deviations in the solar system that, if seen, could have profound consequences for understanding the universe as a whole.
Utilizing reflectors placed on the lunar surface by American astronauts and Soviet rovers, LLR measures the round-trip travel time of short pulses of laser light directed to one reflector at a time. By mapping the shape of the lunar orbit, LLR is able to distinguish between competing theories of gravity. Range precision has improved from a few decimeters initially to a few millimeters recently, constituting a relative precision of 10-9 through 10-11. Leveraging the raw measurement across the Earth-Sun distance provides another two orders of magnitude for gauging relativistic effects in the Earth-Moon-Sun system.
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| The largest of the Apollo lunar laser range reflectors (LLRR) arrays, deployed at Hadley Rille by Scott and Irwin of the Apollo 15 surface expedition in February 1971. The instrument is still a regularly acquired critical part of on-going experimental astrophysics. AS15-85-11468 [NASA/JSC]. |
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| Lunokhod 1 rover in its final parking place (38.315°N, 324.992°E) on the surface of Mare Imbrium. LROC Narrow Angle Camera (NAC) observation M175502049RE, orbit 10998, November 9, 2011, resolution 33 cm per pixel. View original Featured Image released March 14, 2012 (with enlarged inset) HERE [NASA/GSFC/Arizona State University]. |
This review is organized as follows: Section 1 provides an overview of the subject; Section 2 reviews the science delivered by LLR, with an emphasis on gravitation; Section 3 describes current LLR capabilities; Section 4 relates recent surprises from LLR, including the finding of the lost Lunokhod 1 reflector and evidence for dust accumulation on the reflectors; Section 5 treats the modeling challenges associated with millimeter-level LLR accuracy; and Section 6 covers possible future directions for the practice of LLR.
Craters near Lunokhod-1 officially named (July 3, 2012)
The Moon as a platform for astrophysics (April 24, 2012)
A Fundamental Point on the Moon (April 13, 2010)
Lunokhod 1 revisited, too (March 15, 2012)
Long term degradation of optics on the Moon (March 4, 2010)
Dust accumulation on Apollo reflectors and the exosphere (February 16, 2010)
Laser Ranging and the LRO (August 12, 2009)
The continued importance of lunar laser ranging (August 3, 2009)
MacDonald LLR defunded by NSF (June 21, 2009)
New model of lunar motion from Apollo LLRR (December 27, 2008)
Tuesday, July 17, 2012
JAXA announces SELENE-2 now slated for 2017
Tatsuaki Okada, representing JAXA, made reiterated Japan's determination to carry out the SELENE-2 mission at the 39th Scientific Assembly of the Committee on Space Research (Cospar) now underway at Mysore, Karnataka State, in India. According to a report posted by Srinivas Laxman of AsianScientist "nearly 3,000 space scientists from 74 countries are participating in the meeting."
Originally anticipated for a launch in 2012, 2015, and then lost on the budgetary cutting room floor, Okada said Japan's plans for SELENE-2 still included an orbiter, lander and rover.
“While the rocket and the lunar lander will be from NASA," Okada said, according to Laxman, "the astronaut will be from Japan. There will be science exploration and moon utilization by the Japanese astronaut.”
The SELENE-2 design calls an orbiter weighing 700 kg, a lander at 1,000 kg and a small 100 kg rover, though the lander, in line with earlier reports, may have additional capacity for an additional 100 kg payload.
Okada said eleven landing sites were under consideration, including the Fra Mauro region explored by Alan Shepard and Edgar Mitchell of Apollo 14 in 1971. The SELENE-2 lander is not being designed for long-duration stay on the lunar surface, requiring survival through a lunar night. The mission will begin with arrival at local sunrise and come to and end with the loss of solar power at sunset, 14 days later.
Thursday, April 5, 2012
Space Exploration: A Job for Humans
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| Admiral Alan B. Shepard, Jr. (1923-1998), U.S. Navy aviator by profession and cattle farmer by avocation, a few weeks shy of 10 years after becoming the first American in Space. On the afternoon of January 31, 1971 he suits up for only his second space flight, as commander of Apollo 14 and destined to become only the fifth person to explore the surface of the Moon [NASA]. |
Atlantic
The conventional wisdom of space exploration suggests that robotic probes are both more scientifically efficient and cost effective. Not so, argues a professor of planetary science.
When the Space Shuttle Atlantis rolled to a stop in July 2011, NASA bid farewell to the nation's symbol of manned spaceflight. The Obama administration has scrapped NASA's plan to return humans to the Moon by 2020, which was behind schedule because of technical and budgetary problems. As financial constraints threaten the possibility of future ventures into outer space, many in the astronomical community are advocating for the increased use of unmanned robotic space, arguing that they will serve as more efficient explorers of planetary surfaces than astronauts. The next giant leap, then, will be taken with robotic feet.
Dr. Ian A. Crawford thinks it should be otherwise. A professor of planetary sciences at Birkbeck College, London, Crawford makes the case for human space exploration in a new paper entitled Dispelling the myth of robotic efficiency: why human space exploration will tell us more about the Solar System than will robotic exploration alone, published recently in the journal Astronomy and Geophysics. If the goal of space travel is to expand our knowledge of the universe, argues Dr. Crawford, exploration will be most effective when carried out by astronauts rather than robots on the surface of a planet.
Tuesday, February 21, 2012
ESRF X-rays illuminate lunar interior
A science team in the Netherlands claims to have discovered one answer, the natural buoyancy of molten but poorly mixed constituent materials closer to the Moon’s core. The world’s press is reporting their more subtle investigation, using X-rays, with headlines about future lunar volcanism, which contrasts with their own press release and it's secondary headline:
"Scientists have now identified a likely reason for this peaceful surface life: the hot, molten rock in the Moon's deep interior could be so dense that it is simply too heavy to rise to the surface like a bubble in water. For their experiments, the scientists produced microscopic copies of moon rock collected by the Apollo missions and melted them at the extremely high pressures and temperatures found inside the Moon. They then measured their densities with powerful X-rays. The results are published in the Journal Nature Geosciences on 19 February 2012.
"The team was led by Mirjam van Kan Parker and Wim van Westrenen from VU University Amsterdam and comprised of scientists from the Universities of Paris 6/CNRS, Lyon 1/CNRS, Edinburgh, and the European Synchrotron Radiation Facility (ESRF) in Grenoble.
"To determine the density of lunar magma, Wim van Westrenen and his colleagues synthesised moon rock in their laboratory in Amsterdam, using the composition derived from Apollo samples as their “recipe”. The pressures and temperatures close to the core of the Moon are more than 45,000 bar and about 1500 degrees. It is possible to generate these extreme conditions with small samples, heating them with a high electric current while squashing them in a press. By measuring the attenuation of a powerful synchrotron X-ray beam at the (European Synchrotron Radiation Facility) in Grenoble, traversing the sample both solid and molten, the density at high pressure and high temperature could be measured.
"The measurements at the ESRF were combined with computer simulations to calculate the magma density at any location in the Moon.
"Nearly all the lunar magmas were found to be less dense than their solid surroundings, similar to the situation on Earth. There is one important exception: small droplets of titanium-rich glass first found in Apollo 14 mission samples produce liquid magma as dense as the rocks found in the deepest parts of the lunar mantle today. This magma would not move towards the surface.
"Such titanium-rich magma can only be formed by melting titanium rich solid rocks. Previous experiments have shown that such rocks were formed soon after the formation of the Moon at shallow levels, close to the surface. How did they get deep into the mantle? The scientists conclude that large vertical movements must have occurred early in the history of the Moon, during which titanium-rich rocks descended from near the surface all the way to the core-mantle boundary. “After descending, magma formed from these near-surface rocks, very rich in titanium, and accumulated at the bottom of the mantle – a bit like an upside-down volcano. Today, the Moon is still cooling down, as are the melts in its interior. In the distant future, the cooler and therefore solidifying melt will change in composition, likely making it less dense than its surroundings. This lighter magma could make its way again up to the surface forming an active volcano on the Moon – what a sight that would be! – but for the time being, this is just a hypothesis to stimulate more experiments”, concludes Wim van Westrenen."
Reference: Mirjam van Kan Parker, et al., Neutral buoyancy of titanium-rich melts in the deep lunar interior, Nature Geoscience advanced online publication, 19 February 2012
Friday, January 27, 2012
Remnant magnetism hints at once-active lunar core
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| A piece of lunar sample 10020, a rock that appears to carry the signature of a past magnetic field on the moon [NASA]. |
A new study of a lunar rock scooped up by Neil Armstrong and Buzz Aldrin during their Apollo 11 mission indicates that the ancient moon long sustained a dynamo—a convecting fluid core, much like Earth's, that produces a global magnetic field. The age of the rock implies that the lunar dynamo was still going some 3.7 billion years ago, about 800 million years after the moon's formation.
That is longer than would be expected if the lunar dynamo were powered primarily by the natural churning of a cooling molten interior, as is the case on Earth. The moon's small core should have cooled off rather quickly and put an end to any dynamo-generated magnetic field within a few hundred million years. So researchers may have to explore alternate explanations for how a dynamo could be sustained—explanations that depart from thinking of the lunar interior in terms of Earthly geophysics.
A standard-issue, Earth-like dynamo "would have died out on the moon much, much before 3.7 billion years ago," says Erin Shea, a graduate student in geology at the Massachusetts Institute of Technology and lead author on a study in the January 27 issue of Science. "We have to start thinking outside the box about what generates a lunar dynamo."
A lunar sample collected by Apollo astronauts suggests that other-Earthly geophysics drove the moon's churning interior
A similar paleomagnetic study in 2009 by some of Shea's co-authors demonstrated the presence of a lunar dynamo some 4.2 billion years ago. That is just at the cusp of what would be possible with an Earth-like dynamo driven by a cooling interior alone. "Even then it's not trivial," says Ian Garrick-Bethell, a planetary scientist at the University of California, Santa Cruz (U.C.S.C.), who was the lead author of the 2009 study.
Thursday, September 8, 2011
On the rim!
Mark Robinson
Principal Investigator
Lunar Reconnaissance Orbiter Camera
Arizona State University
The 6 September 2011 LROC Featured Image described the special low orbit month that allowed LROC to snap its highest resolution images of the Apollo 12, 14 and 17 landing sites. That post featured the Apollo 17 site, while today's Featured Image looks in detail at the Apollo 14 image.
In February 1971 Edgar Mitchell examines the map, looking for landmarks, as he and Alan Shepard work to find the rim of their goal, Cone crater. It would later be determined (and LROC would confirm) that the Apollo 14 astronauts were very close.
What can we see better at the Apollo 14 site compared to previous images (9 August 2009, 4 February 2011)? The increased resolution allows indentification of the astronaut backpacks (PLSS), the small two wheeled cart (Modularized Equipment Transporter or MET) that the astronauts used to transport tools and samples, and the high gain antenna (HGEA). You can also make out one of the LM legs at the 7 o'clock position on the descent stage. The pixel size of the NAC image is not high enough that all these objects can be resolved, but rather we can detect that they are there. Only through comparison with surface photography can we definitively identify the smaller objects left by the astronauts. With the smaller pixel size we can begin to resolve the descent stage, we can see its shape, brightness differences on the deck, and footpads.
New LROC low orbit image of the Apollo 14 Lunar Module descent stage. (See a comparable view as seen by the astronauts HERE.) Upper two panels show new image but with different contrast stretches, and the lower image is an enlarged version. Each scene is 75 meters wide, north is up, Sun is from the west (left). [NASA/GSFC/Arizona State University].
The traverse up Cone crater was the main science goal for Al Shepard and Ed Mitchell. Impact craters spread out ejecta in a very predictable manner. The outer edges of the ejecta are mostly composed of material from or near the surface where the bolide (asteroid or comet) impacted, while the ejecta at the rim of the crater comes from deepest regions within the crater. So it is a "simple" matter of walking towards the crater and collecting samples to reconstruct an accurate picture of the original subsurface. Well simple in principle.
LROC NAC low orbit image of Cone crater, near the Apollo 14 landing site. Image is 400 meters wide, north is up, Sun is from the west (left). View the full-size image HERE [NASA/GSFC/Arizona State University].
The astronaut trails are not so distinct near Cone crater. Here the astronauts were out of the area that was scoured by the descent stage engine upon landing. The scouring produced a distinct bright halo at all the landing sites, most likely due to the finest particles being blown away from the spot just below the engine in the final seconds of landing. These bright particles were dispersed more or less evenly around the Lunar Module creating the halo effect. As astronauts walked around they kicked upper darker soil from beneath the halo creating distinct trails. Outside of the halo the soil kicked up may not have had as much contrast and is thus harder to spot.
Be sure to watch our movie describing the landing site!
Explore Cone crater in our Browse Gallery.
Apollo 14 at 25 cm per pixel


For point by point comparison, here's the view out the starboard window of the Apollo 14 lunar module Antares following the end of Shepard and Mitchell's second EVA. The trail west to the ALSEP package, deployed near the horizon at upper left, stands out in the latest LROC NAC image release, together with many of the items nearby. View the full size version HERE [NASA/ASJ/LP].
Apollo 14 landed near Fra Mauro crater in February 1971. On the first moon walk, the astronauts set up the lunar monitoring equipment known as the Apollo Lunar Surface Experiments Package (ALSEP) to the west of the landing site and collected just over 42 kilograms (about 92 pounds) of lunar samples. Luckily for them, they had a rickshaw-style cart called the modular equipment transporter, or MET, that they could use to carry equipment and samples.
The labeled version of the latest survey of the Apollo 14 landing site by the Lunar Reconnaissance Orbiter Camera system [NASA/GSFC/Arizona State University].
› Larger image
› Larger image (unlabeled)
Related Materials:
LRO Briefing: Latest images of the Apollo landing sites
LROC: Skimming the Moon
NASA: NASA Spacecraft offers sharper views of Apollo landing sites
Highest Resolution Video from Goddard Space Visualization Studio (SVS)September 6, 2011
Friday, August 19, 2011
LROC: Ray of boulders
Lillian Ostrach
LROC News System
Take a peek at the full LROC NAC image - can you find reflectance variations within the ejecta blanket that may represent compositional differences from within the crater? Do you see any other bouldery ejecta rays around the rim?
Related Posts:
Ejecta Blanket Features
Scouring secondary ejecta
Dark haloed crater in Mare Humorum
Slice of Mare
Small crater in Oceanus Procellarum
Tuesday, July 5, 2011
DOJ files suit against Edgar Mitchell for DAC camera
If the government throws a camera away on the moon and an astronaut then picks it up and saves it, does it become his to own and sell?
That's more or less the question the U.S. government is seeking a federal court answer in the case "United States of America vs. Edgar Mitchell," which was filed in Miami, Florida last Wednesday.
The lawsuit, which names the sixth man to walk on the moon as the defendant, asks the court to declare a movie camera that was used during the 1971 Apollo 14 mission as the "exclusive property of the United States."
After returning to Earth with the camera and having it in his possession for the past four decades, Mitchell, 80, attempted to sell it last month through a New York auction house. The camera, which was estimated to sell between $60,000 and $80,000, was withdrawn before its sale could proceed.
Wednesday, April 27, 2011
Ambassador of Exploration Award award goes to Alan Shepard
Daniel Baxter
AvStop.com
Shepard's family members will accept the award on his behalf during a ceremony at 5:30 p.m. EDT on Thursday, April 28, at the U.S. Naval Academy Museum, located at 74 Greenbury Point Road in Annapolis, Md.
His family will present the award to the museum for permanent display. NASA's Chief Historian Bill Barry will represent NASA at the event, which will include a video message from agency administrator Charles Bolden.
Shepard, a 1945 graduate of the Naval Academy, was one of NASA's original seven Mercury astronauts selected in April 1959. On May 5, 1961, he was launched from Cape Canaveral, Fla., aboard the Freedom 7 spacecraft on a suborbital flight that carried him to an altitude of 116 miles.
Shepard made his second spaceflight as the commander of Apollo 14 from Jan. 31 to Feb. 9, 1971. He was accompanied on the third lunar landing by astronauts Stuart Roosa and Edgar Mitchell.
Friday, February 4, 2011
New View of Apollo 14: 40th Anniversary
Mark RobinsonPrincipal Investigator
Lunar Reconnaissance Orbiter Camera
Arizona State University
Think of the Apollo sites as benchmarks put in place four decades ago for the LROC team!
When will we return to the Moon?
Ed Mitchell took this splendid picture after he and Al Shepard jettisoned the PLSSs in preparation for launch. Of particular interest are the tracks made by the crew and the MET during the traverse to the ALSEP deployment site and during the return to the LM. Apollo 17 astronaut Jack Schmitt speculates that the descent plume sweeps away the fine particles of soil, leaving a surface dominated by small rock fragments that reflect sunlight from the down-Sun direction and make the surface look lighter in color than normal. In places where the surface is disturbed, the normal reflectivity of the surface is restored. Whatever the detailed explanation for this phenomenon, it is related to the fact that, from orbit, the area immediately surrounding a LM looks noticeably lighter in color. The ALSEP Central Station is about 180m from the LM. Note the excursions the crew made around the rimless crater in the foreground and the large depression in the middle distance that they traversed in both directions. Without the visual clues provided by the tracks, the depression is not easy to pick out in this down-Sun photo. Note that the flag is now pointing on an azimuth of about 335 and undoubtedly moved from it prior pointing of about 120 as a result of the cabin depressurization done for the jettison."
Read our previous LROC Apollo 14 posting.
Monday, January 31, 2011
Forty years ago - America's 2nd Return to Space
Friday, July 16, 2010
Moon walk led to 'deep' frontier
Jim Wise
The Durham News
The sixth human to walk on the moon, Mitchell is a native of Hereford, Texas, and earned his doctorate in aeronautics and astronautics at MIT.
While in graduate school, he became interested in the research in "extra-sensory perception" pioneered by Duke University Prof. J.B. Rhine. Mitchell met and corresponded with Rhine and, while in space, conducted ESP experiments of his own which, he says, had positive results similar to those Rhine had had on Earth.
Mitchell was originally assigned to the ill-fated Apollo 13. Switched to the later mission, he and fellow astronaut Ken Mattingly simulated the roles of command and lunar module pilots during the efforts that brought Apollo 13's crew home safe.
During his own flight home, Mitchell had a mystical experience that radically changed his career.
"It was accompanied by this bliss, or ecstasy - a 'wow' experience," he said later.
According to his Website Mitchell "became engulfed by a profound sensation "a sense of universal connectedness. He intuitively sensed that his presence, that of his fellow astronauts, and that of the planet in the window were all part of a deliberate, universal process and that the glittering cosmos itself was in some way conscious."
Mitchell retired from NASA in 1972 and founded the Institute for Noetic Sciences to sponsor research into the nature of consciousness as it relates to cosmology and causality. He is also a strong advocate for changing humans' attitude toward the earth and for protecting its resources.
On Friday, he is speaking on "Sustainability" at the Duke Center for Living. His appearance is sponsored by the Rhine Research Institute, which J.B. Rhine established upon retiring from Duke in 1964. His talk is open to the public.
Tuesday, February 16, 2010
Dust accumulation on Apollo laser reflectors may indicate a surprisingly fast and more dynamic lunar exosphere
Joel Raupe
Lunar Pioneer
Though Conrad and Bean succeeded also in collecting the camera and shovel arm from the unmanned Surveyor 3, learning what those artifacts could tell us about the Moon as a "long duration exposure facility" was not a NASA priority. The Final Reports in 1970 (NASA-CR-121796) indicated after careful examination of Surveyor 3's components that what slight "weathering" there was to be found on camera was wholly a result of the blast of Apollo 12 descent engine. But, first actually locating and then landing the lunar module precisely where Surveyor 3 was situated (there were no orbital photographs of the spacecraft in situ) was pretty astonishment by itself. No one was cautious of any evidence of an active fallout of electrostatic dust on the Moon in 1969.
Though there had been hints of a gossamer-thin migratory dust phenomena happening on the Moon, Apollo 8 crew sightings from orbit and night time Surveyor images, the concerns of the time were solar and cosmic radiation, and micrometeor bombardment. Evidence at the Apollo astronaut's feet and on their spacesuits (and in their eyes and noses) of the voluminous accumulations of dust everywhere on the Moon was (not incorrectly) thought to be the end result of extremely slow processes.
The evidence for the presence of a dusty lunar exosphere has mostly been discovered to explain gathering evidence, not all of it gathered on location. Twenty years ago great (but very thin) trailing clouds of silicon and potassium ions, among the more easily spectographically-detected dusty elements. These were composed into photographs showing the Moon orbiting Earth in a cloud of it's own bombardment.
The forty years since Apollo, occasionally punctuated with influential, if rare (until 2007), lunar probes like Lunar Prospector, gave lunar and planetary scientists a lot of time and new evidence to ponder. Perhaps the length of time itself allowed many theories to be shaken out and ultimately proven amazingly accurate.
Departing tests of instruments now used by Cassini at Enceladus to detect water were aimed at first light at the Moon, precisely because its bone-dryness was believed to present a sold baseline of zero water. The unexpected detection of water there, coincident with daily cycles of sunlight, has now become part of the context of evidence old and new that verified the astounding conclusion that some areas of the lunar surface may be wetter than Mars (relatively speaking).
In May 2012 NASA Lunar Atmosphere and Dust Environment Explorer (LADEE) should have the capability needed to improve our understanding of processes related to the charging of lunar dust particles and the implantation and presence of water on the Moon, the interaction of solar particles and energetic photons (including neutral hydrogen) that polarize the smallest grains on the Moon's immediate surface. Gardened over, roughly every 2 million years predominately by micrometeorite bombardment, submicron sized flecks are repelled by opposing charges into ballistic trajectories as high as the orbit forty years ago of Apollo's command and service modules.
Though posing little or no danger to orbiting spacecraft, the range of hazards that lunar dust poses to sustained surface operations, whether manned of unmanned, are manifold. The susceptibility of the smallest of these shards to electrical charging, their stubborn clinging to seals and skin, for example, is both the source of their danger and perhaps their mitigation.
The forensics done on the Surveyor 3 parts offered us lessons. In the near future, if anything is to be learned about fallout of lunar dust from an examination of human artifacts a degree of care must be taken beyond the mission goals of Apollo 12. If you want to approach and examine Apollo 11's descent stage, for example, the arrival of Apollo 12 near Surveyor 3 showed any similar arrival near near Tranquility Base should be from well over the horizon, and more. Calculations show at least some of the famous dust raised at the arrival and departure of Apollo's lunar modules must have attained great altitude, even escape velocity.
Very little would be needed to disturb a forty year record of dusty "precipitation."
It is thought that the migratory dust circling the Moon continuously, with its wave crest directly behind the longitude of sunrise, is related to the forces that lead to implantation of volatile molecules like hydroxyl and water. The path of the oppositely charged and neutralized dust fallout, it's cycle of return to the surface, may rain in one direction during the equivalent of a lunar winter and predominate in the opposite deviation from westerly during a lunar summer.
Dust fallout cycles may then be the source of the criss-crossed "elephant skin" patterns seen on lunar high places and elsewhere.
Tied as the phenomena is to solar-induced charging, the pattern of the Moon's dusty cycles of levitation and fallout are attenuated during the Moon's monthly transit through Earth's magnetotail. Something similar may be true, on a smaller scale, affecting levitation and subsequent fallout of lunar dust in and around especially strong crustal magnetism. This might perhaps then be a solution to the mystery posed by a presence of brighter surface albedo (low optical maturity) characteristic of lunar swirls within these"magnetic anomalies" whose origins otherwise speak of greater age than high albedo would indicate.
And now, very recently, evidence comes to "light" that fallout from the very thin, neverending lunar dust storm is accumulating with a greater speed than anyone may have imagined.
When a powerful laser is aimed at the Moon from Apache Point in New Mexico, the thin beam consisting of many hundreds of billions of photons spreads out to at least two kilometers in width during the second and a half needed for it to center on Apollo's retroreflectors, 400,000 kilometers away. The small sampling of that beam reflected back is literally counted in single photons by the time it returns back to New Mexico.
After accounting for things like today's more accurate photon detectors, more powerful and accurate lasers, more suitable laser wavelengths and a more powerful telescopes than originally used for this purpose at MacDonald Observatory in Texas, the photon count should be measurably improving, just as it has been. Still, something doesn't quite add up, and one investigator thinks he knows why.
"Tom Murphy from the University of California, San Diego, who leads one of the teams at the Apache Point Observatory in Sunspot, New Mexico, thinks the mirrors have become coated in moon dust. "The lunar reflectors are not as good as they used to be by a factor of 10," he says."
Saturday, January 30, 2010
LROC: Precise 3D Measurements of Objects at the Apollo 14 landing site using LRO's Narrow-Angle Camera stereo images

Traverse map of Apollo 14 landing site. [NASA/GSFC/ASU/OSU] (Full Size HERE.)
Jordan Lawyer
LROC News System
In the zoomed image (HERE), the lunar module can be identified by its deck (red points) and distinctive shadow (green lines). These points are measured in the two stereo images and their corresponding 3D ground coordinates are computed. Note that the shadow analysis uses different times and sun angles of the two images for computation. In addition, the nearby terrain is measured at the selected points on the ground (green points) as a reference. From these measurements, we can compute the height and diameter of the lunar module. As the result, the height of the lunar module (descent stage) is estimated as 3.0 m, compared to the design specification of 3.2 m. On the other hand, the shadow analysis resulted in a height of the lunar module of 3.2 m. Furthermore, using a least squares fitting to a circle the diameter of the lunar module is computed as 4.4 m, compared to the design data of 4.2 m.

Friday, October 9, 2009
Making an Impact (40 years ago)
LROC News System
A distinctive crater about 35 m in diameter was formed when the Apollo 14 S-IVB (upper stage) was intentionally impacted into the Moon. The energy of the impact created small tremors that were measured by the seismometer placed on the Moon by Apollo 12 astronauts.
The interior of the crater has bright mounds and a bright ejecta blanket surrounds the exterior of the crater. Bright rays are observed to extend across the surface for more than 1.5 km from the impact. This image was taken when the Sun was relatively high in the sky (illumination angle of 25.1°) bringing out subtle differences in albedo (reflectivity or brightness). The Apollo 16 spacecraft first photographed this crater (Pan Camera frame 5451) and scientists noted the unusual occurrence of dark rays mixed with bright rays. Can you find the dark rays?
The upcoming LCROSS impact into Cabeus will also be used to probe the lunar subsurface. The Apollo 14 impact was used to send vibrations through the surface to help scientists study the internal structure of the lunar crust, the LCROSS impact will throw materials up into space so compositional measurements can be made of the subsurface from a trailing spacecraft and Earth-based telescopes.
The Apollo impact velocity was 2.54 km/sec and an angle of 69° from the horizontal along a heading of 103° (west to east). The S-IVB had a mass of 14,016 kg (30835 lbs) at the time of impact and impact energy was 5.54 x 1010 J (equivalent to just over 10 tons of TNT). The signal from the impact was recorded on the Apollo 12 seismometer; it lasted for about 3 hours. The LCROSS impactor (Centaur upper stage) is much smaller than the S-IVB and thus will make a smaller crater. The Centaur weighs about 2000 kg and will impact with a velocity of about 2.5 km/sec.
Roam around in the full NAC image comparing the S-IVB impact crater with others nearby.Friday, August 21, 2009
Lasting boot prints from 1971
A better look, from a slightly higher solar phase angle: The moon-boot prints of the first American in Space, the late Admiral Alan Shepard and Apollo 14 lunar module pilot Edgar Mitchell appear unchanged since they climbed the slope, searching for the rim of Cone Crater on the Fra Mauro formation in February 1971. The tracks of the two men on their second of two EVA's, along with those of the wheeled Modular Equipment Transporter (MET) drug behind them, lead off to the upper right, as recommended in the full image."A month has already passed since LROC acquired its first images of the Apollo landing sites. In this time the Moon completed one rotation beneath LRO’s orbit, thus providing another set of overflights. Because LRO is not in synch with the lunar day we see the same ground with different lighting – this time the Sun is 24 degrees higher above the horizon providing a clearer view with fewer shadows. Albedo contrasts are greater, and more clearly show soil disturbances from landing, astronaut surface operations, and blast off."
"Apollo 14 Astronauts Alan Shepard and Edgar Mitchell explored the Fra Mauro highlands, which are composed of ejecta from the massive Imbrium impact..."
"During the second EVA, the astronauts performed what is known as a “radial traverse” across the ejecta field and up to the rim of Cone crater. When impact craters form, rocks excavated from the deepest parts of the crater fall near the rim; surface rocks end up away from the crater. Thus, as explorers move up a crater's ejecta blanket, they can sample a complete stratigraphic section of geologic materials providing priceless insights about the composition and nature of the lunar subsurface. Think of an impact crater as a natural roadcut exposing rocks from depth. In this LROC image, you can follow nearly the whole path walked by the two astronauts. The term “radial traverse” does not quite do the crew of Apollo 14 justice. Their journey sounds like a stroll in the park, however the reality is quite the contrary. The hike up Cone crater was quite challenging. For the first time, astronauts traveled out of the sight of their lunar module while hiking uphill over 1400 meters with only a poor map, dragging the tool cart (MET), and wearing their bulky spacesuits. It was an amazing feat that the two astronauts made it to the top of Cone ridge and acquired all their samples. They ended up about 30 meters shy of peering into Cone crater itself, surely a disappointment at the time, but absolutely no reflection on the success of the traverse and the scientific results gleaned after the mission."
Friday, July 17, 2009
Finally...
Still very early in the calibration phase of what will be its long-awaited two-year mission exploring the Moon, Arizona State University's stewards of the LRO wide and narrow angle camera system have delivered just preliminary photographs of five of the six Apollo lunar module descent stages (which turned out situated precisely where they were supposed to be when left behind almost forty years ago.
Naturally, the Lunar Pioneers can't think of a better way to celebrate the accomplishment of Apollo 11. (The intensive tracking left behind by the boots of Alan Shepard and Edgar Mitchell on Fra Mauro in February 1971 can easily be seen, having left an obvious trail between the ALSEP and Antares.)
LROC Site Link HERE.
Five Apollo landing sites photographed
All six manned lunar landing missions took place at or soon after local lunar sunrise, so the long shadows fall away close to the direction from which they arrived.
The Apollo 12 site, around 100 meters from the earlier landing site of Surveyor 3, is expected to be photographed in coming weeks.
"The LROC team anxiously awaited each image," said LROC principal investigator Mark Robinson of Arizona State University. "We were very interested in getting our first peek at the lunar module descent stages just for the thrill -- and to see how well the cameras had come into focus. Indeed, the images are fantastic."



























