Showing posts with label Apollo 14. Show all posts
Showing posts with label Apollo 14. Show all posts

Saturday, February 6, 2016

Edgar Mitchell (1930-2016)

Edgar Mitchell, sixth human to visit the lunar surface, takes a live panorama of the close horizon using the first color television camera successfully operated on the Moon; at Fra Mauro, south of Copernicus, February 1971. Photograph by Apollo 14 commander Alan Shepard [NASA/JSC].
Astronaut Edgar Mitchell, lunar module pilot on Apollo 14, passed away Thursday in West Palm Beach, Florida,  and on the eve of the 45th anniversary of his lunar expedition in 1971.

Mitchell joined Apollo 14 commander Alan Shephard, Jr., the first American in space, in the lunar module Antares, which touched down February 5, 1971, in the Fra Mauro highlands. Shepard and Mitchell were assigned to traverse the lunar surface to deploy scientific instruments and perform a communications test on the surface, as well as photograph the lunar surface and any deep space phenomena. It was Mitchell’s only spaceflight.

Mitchell and Shephard set mission records for the time of the longest distance traversed on the lunar surface; the largest payload returned from lunar surface; and the longest lunar stay time (33 hours). They were also the first to transmit color TV from the lunar surface. Mitchell helped collect 94 pounds of lunar rock and soil samples that were distributed across 187 scientific teams in the United States and 14 other countries for analysis.

Read the full NASA release HERE.

Tuesday, November 19, 2013

Lunar Laser Ranging: The Millimeter Challenge

Lunar Laser Range Reflector arrays
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].
T. W. Murphy, Jr.
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.

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].
As LLR precision has improved over time, the technique has remained at the cutting edge of tests of gravitational phenomenology and probes of the lunar interior, and has informed our knowledge of Earth orientation, precession, and coordinate systems. LLR was last reviewed in this series in 1982; this update describes the key science drivers and findings of LLR, the apparatus and technologies involved, the requisite modeling techniques, and future prospects on all fronts.

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].
LLR is expected to continue on its trajectory of improvement, maintaining a leading role in contributions to science. Other recent reviews by Merkowitz (2010) and by Muller, et al. (2012) complement the present one. The Merkowitz review, like this one, stresses gravitational tests of LLR, but with greater emphasis on associated range signals. Next-generation reflector and transponder technologies are more thoroughly covered. The Muller et al. review (for which this author is a co-author) covers a more complete history of LLR, has statistics on the LLR data set, and provides greater emphasis on geophysics, selenophysics, and coordinate systems.

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.

Tuesday, July 17, 2012

JAXA announces SELENE-2 now slated for 2017

Japan's SELENE-2 follow-up to the versatile Kaguya (2007-2009) orbiter has remained essentially the same in design since originally proposed. Participation by Japan's experienced astronaut corp in any future manned mission to the Moon carried out by the United States government may now be some distance beyond 2017 [JAXA].
A representative of Japan's space agency JAXA announced Sunday in India that planning is definitely underway to launch the long-anticipated sequel mission to that nation's first lunar orbiter, "Kaguya" (SELENE-1) in 2017. Because budgeting for the mission has been "delayed" twice through Japan's own sovereign debt difficulties news that JAXA has not abandoned the mission design is encouraging.

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. 

“It is for developing and for the demonstration of key technologies for future human exploration," Okada said. "It is a multipurpose mission which is a precursor for human exploration,” he told a Cospar session on lunar sciences. Okada later told Asian Scientist Magazine a future manned lunar mission "will be in collaboration with NASA."

“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.”

Okada also, according to Laxman, "did not rule out SELENE-2 being delayed once again, because of budgetary constraints."

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

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].
Jared Keller
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.

Read the feature article HERE.

Tuesday, February 21, 2012

ESRF X-rays illuminate lunar interior

Image of artificial moon rock sample, measuring about half
millimeter across, made with an electron microprobe at ambient
temperature after the experiment with X-rays. The fragmenta-
tion of the sample occurred when it was extracted from the
small diamond cylinder in which it had been melted under high
pressure and temperature [ESRF/Nature].
Does the Moon still have even a small, warm liquid core? The answer can only be apparent indirectly, behind its dance movements and the combined angular momentum of it juggled components; the Moon’s anisotropy. If, as investigators now claim, the Moon’s outer surface is still shrinking or, in some cases, stretching, other outward evidence of even a small warm and liquid core can only be discovered indirectly. Why, for example, is any evidence of volcanism on the Moon’s surface at least a billion years old?

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:

Deep lunar magma is too heavy to produce active volcanoes

"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.

Exploded schematic of the high-pressure cell
assembly for the ESRF synchrotron  X-ray
experiment. The artificial moon rock samples
(orange) were placed inside the ring-shaped, natural
diamond sample holder (grey), and surrounded by
a large disk-shaped container (red) [ESRF/Nature].
"The driving force for vertical movement of magma is the density difference between the magma and the surrounding solid material, making the liquid magma move slowly upwards like a bubble. The lighter the liquid magma is, the more violent the upward movement will be.

"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.

 “We had to use the most brilliant X-ray beam in the world for this experiment because the magma sample is so tiny and confined in a massive, highly absorbing container. Without a bright beam of X-rays, you cannot measure these density variations”, says Mohamed Mezouar from the ESRF.

"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

A piece of lunar sample 10020, a rock that appears to carry
the signature of a past magnetic field on the moon [NASA].
John Matson
Scientific American

The moon of today is a static orb with little to no internal activity; for all intents and purposes it appears to be a dead, dusty pebble of a world. But billions of years ago the moon may have been a place of far more dynamism—literally.

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
Using a high-resolution magnetometer, the researchers found that the lunar sample indeed formed in the presence of a magnetic field, perhaps even one as strong as Earth's magnetic field today. "What this sample tells us is that at some point the moon did have a dynamo," Shea says. "This magnetic field lasted much longer than we had considered before."

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.
Read the full online article HERE.

Thursday, September 8, 2011

On the rim!

Saddle rock, so close! Apollo 14 astronauts hiked up the flanks of Cone crater and got as far as Saddle rock before they had to turn back. A few tens of meters and what a view! LROC image 25 cm pixel scale, image 200 meters wide, LROC Narrow Angle Camera observations M168319885, LRO orbit 9939, September 4, 2011; north is up. View the full size LROC Featured Image HERE [NASA/GSFC/Arizona State University].

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].
Imagine hiking up the flanks of Cone crater with no compass (the Moon does not have a magnetic field so a compass is useless), only a very general map, carrying a heavy backpack, dragging a small wheeled cart loaded with tools, restricted vision from inside a helmet, and very strict time constraints! Al and Ed made it as close as  Saddle rock, which is only about 20 or 30 meters from the rim! However, the astronauts did not know they were that close. During the traverse they were temporarily bewildered as to their exact location. As it turns out, while they met 100% of the geologic sampling goals, they just missed out on the spectacular view into Cone crater.

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.
See Cone Crater!

Apollo 14 at 25 cm per pixel


Inset from low altitude view of the Apollo 14 landing site, released by NASA September 6, 2011. The LROC Narrow Angle Camera (NAC) were put to use during a month-long change in orbit that lowered LRO down to as little as 22 km over the Moon. The paths left by astronauts Alan Shepard and Edgar Mitchell in February 1971 on both Apollo 14 moon walks are visible. (At the end of the second moon walk, Shepard famously hit two golf balls.) The descent stage of the lunar module Antares is also visible [NASA/GSFC/Arizona State University].


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


Dozens of boulders, ranging from 10 to more than 30 meter in diameter, are distributed within an ejecta ray close to a crater rim (lower right) located inside the Mare Moscoviense basin (32.52°N, 143.625E°). These boulders represent the deepest material excavated during the crater's formation. From a montage of LROC Narrow Angle Camera (NAC) observations M159013302L & R, field of view is roughly 850 meters; LRO orbit 8568, May 2, 2011. View the full-size LROC Featured Image HERE [NASA/GSFC/Arizona State University].

Lillian Ostrach
LROC News System

Northeast of Mare Moscoviense, an unnamed Copernican-aged crater has an extensive ejecta blanket (32.56°N, 143.53°E, diameter ~6 km). The ejecta blankets of impact craters provide a useful tool toward relative age dating and the formation of a geologic story for a region when using remotely sensed image data. The presence of a rayed, continuous ejecta blanket surrounding an impact crater indicates that the crater formed relatively recently in lunar geologic time. The distribution of ejecta around the crater can help predict whether the bolide impacted obliquely and from which direction it came. Moreover, if there are reflectance variations in the ejecta blanket, the impact may have exposed material of multiple compositions, and how bouldery or smooth an ejecta blanket appears may help scientists hypothesize the physical properties of the target material (e.g., solid rock, granular regolith, or a combination of both).


LROC Wide Angle Camera (WAC) monochrome mosaic context image of the unnamed crater, northwest of Mare Moscoviense. Asterisk designates the area of LROC Featured Image, released August 18, 2011. See the full-sized version HERE [NASA/GSFC/Arizona State University].


Another WAC image, a 604 nm band mosaic from September 12, 2010, when the local sun was higher and when relief gives way to finer albedo subtleties, demonstrates why this small crater is relatively easy to pick out in small-scale farside imagery. The north shore of "the Sea of Moscow" itself, the floor of the larger impact basin, is just beyond the hills etched by the impact, to the south [NASA/GSFC/Arizona State University].

Ejecta blankets can also provide human explorers an easy means to sample lunar material from depth. Because impact events displace material in a ballistic trajectory from the point of impact, the vertical stratigraphy of the rocks and regolith are exposed within the ejecta blanket in a horizontal manner. Does this make sense? Think about it: when a bolide impacts the surface, the surface regolith is the first material ejected and will travel the farthest. As the energy from impact is dispersed, more material is ejected from the rapidly-forming impact crater, continuing to form the ejecta blanket. The last bit of material ejected will be from the deepest part of the crater and deposited near the crater rim - exactly like those boulders seen in the opening image. What a concept - the ability to create a vertical cross section of an area simply by moving through an ejecta blanket on the surface!


In this smaller-scale, 400 kilometer field of view of a WAC montage released in 2010, stitched from observations at local afternoon illumination, a good mix of relief and albedo features can be seen. The bright crater and its rays, shaped by the anatomy of the landscape where it formed, begin to blend together at this scale [NASA/GSFC/Arizona State University].


Even in this section taken from a full hemisphere-scale (1600 meter resolution) image of the Moon's farside the area affected by the bright crater's albedo stands out like a star, north of Mare Moscoviense. View the hemisphere-wide LROC WAC montage HERE [NASA/GSFC/Arizona State University].

This concept, using radial traverses of an ejecta blanket to sample vertical stratigraphy, was tested both in the laboratory during the 1960s and by Apollo 14 in 1971. Astronauts Alan Shephard and Edgar Mitchell attempted to reach the Cone crater rim and sampled the ejecta blanket at various locations during their traverse. Unfortunately for them, the gently undulating landscape around Cone crater obscured the crater rim from view and they were forced to return from their traverse without photographing the interior of the crater. However, later analysis of photography from the traverse, paired with orbital images, revealed that they had nearly reached the rim! The astronauts were closer than 30 meters from the crater rim, so their samples probably represent the deepest material excavated by the impact. This experience - and experiment - showed that a radial traverse of crater ejecta was an appropriate method to sample the vertical stratigraphy. The high-resolution LROC NAC images, coupled with derived DTM topography will ensure that future human lunar explorers make it to the crater rim when making a radial traverse of an ejecta blanket!

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

CollectSPACE.com

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.

Read the story, HERE.

Wednesday, April 27, 2011

Ambassador of Exploration Award award goes to Alan Shepard


Admiral Alan Shepard (1923-1998), the former Naval Aviator commands Apollo 14, his second spaceflight since becoming the first American in space during a 15 minute flight in 1961 [NASA/Apollo 14 Surface Journal].

Daniel Baxter
AvStop.com

NASA will posthumously honor Alan B. Shepard Jr., the first American astronaut in space and who later walked on the moon, with an Ambassador of Exploration Award for his contributions to the U.S. space program.

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.

Read the full story HERE.

Friday, February 4, 2011

New View of Apollo 14: 40th Anniversary


LROC Narrow Angle Camera (NAC) observation M150633128 of the Apollo 14 landing site acquired January 25, 2011 (LRO orbit 7334; resolution = 0.5m). The Descent Stage of the lunar module Antares is at center and the foot paths trailed by Shepard & Mitchell in February 1971 seem totally undisturbed since their departure forty years ago this weekend (field of view 500 meters). Experience the full-sized (1000x1000) LROC Featured Image released February 4, 2011 HERE [NASA/GSFC/Arizona State University].

Mark Robinson
Principal Investigator
Lunar Reconnaissance Orbiter Camera
Arizona State University


The LROC Narrow Angle Cameras continue to image the Apollo landing sites as the mission progresses. Every time LRO passes overhead the Sun is at a different position so each image gives a different perspective. Repeat imaging also serves LROC cartographic goals. Since the position of the lunar modules and other pieces of hardware are very accurately known the LROC team can check the accuracy of the mission-provided ephemeris.

Think of the Apollo sites as benchmarks put in place four decades ago for the LROC team!


Close-up showing the Apollo 14 Lunar Module's Descent Stage (right) and Apollo Lunar Surface Experiment Package (ALSEP - arrow) with tracks between the two landmarks by Shepard & Mitchell still fresh and distinctive almost precisely 40 years later. In that interval since their departure the foot prints and Apollo 14's deployed materials endured 534 lunar days and nights of relentless exposure, adding to their immeasurable value as sentinel recorders of the lunar environment [NASA/GSFC/Arizona State University].

The Apollo 14 astronauts explored the surface of the Moon on February 5th and 6th, 1971, 40 years ago this weekend. Much was learned during the Apollo missions, yet most of the history and geology of the Moon remains a mystery.

When will we return to the Moon?


Apollo 14 Post EVA view by Edgar Mitchell from inside Antares looking west toward the ALSEP station. LROC PI Mark Robinson suggests matching Edgar Mitchell & Alan Shepard's tracks in this photograph with those in the new LROC NAC view swept up from LRO orbit overhead on January 25, 2011 - forty years later. View the full-resolution high-defintion version of Mitchell's photograph HERE [AS14-66-9338 - NASA/Apollo Surface Journal].

From the Apollo Surface Journal, Apollo 14 Image Library (Magazine 66) "
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."

No one to ask for directions: Apollo 14 lunar module pilot Edgar Mitchell finds the "ground truth" of hiking on the Moon, that things can look very different on the surface than from Lunar Orbiter photography from orbit, and he surveys a map while looking for landmarks. Meanwhile Alan Shepard takes his picture near the end of their unsuccessful ascent up the gentle slope to Cone Crater, at Fra Mauro, February 1971. (It was the first time an Apollo expedition had journeyed beyond view of their spacecraft) [AS14-64-9089HR/NASA/ASJ].



A 'true-color' HDTV orbital view, from Japan's SELENE-1 (Kaguya), of the ancient Fra Mauro crater group and material spilled onto this area, south of Copernicus, from the epoch-marking basin-forming impact formimg Mare Imbrium to the northwest ~3.8 billion years ago. The landing site of Apollo 14 is located in the low hills north of the largest of these craters, at upper center. Click HERE for the full-sized original image release [JAXA/NHK/SELENE].

Monday, January 31, 2011

Forty years ago - America's 2nd Return to Space

America's 2nd "Return to Space," January 31, 1971
Apollo 14, with Alan Shepard, Edgar Mitchell & Stu Roosa onboard, departs Kennedy Space Center for the Moon  nine months after the nearly-disastrous Apollo 13 mission. For Admiral Shepard, America's first astronaut, it had been a longer wait. 10 years had passed since that first 15 minute suborbital flight of the Mercury program. After being grounded for an inner ear condition, now in command of only his second (and last) spaceflight, Apollo 14 would become the only flight to the Moon made by any of the "Original Seven." [NASA/ASJ].

Friday, July 16, 2010

Moon walk led to 'deep' frontier


Apollo 14 lunar module pilot Edgar Mitchell surveys their map and looks for landmarks as Cmdr. Alan Shepard takes his picture, near the end of their unsuccessful walk to Cone Crater at Fra Mauro, February 1971. It was the first time an Apollo expedition had journeyed beyond view of their spacecraft [AS14-64-9088HR/NASA/ASJ].

Jim Wise
The Durham News

In February 1971, U.S. Navy Capt. Edgar Mitchell was lunar module pilot on Apollo 14, the third U.S. mission to land on the moon.

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.

Read the Article, HERE.

Tuesday, February 16, 2010

Dust accumulation on Apollo laser reflectors may indicate a surprisingly fast and more dynamic lunar exosphere



February 5, 1971 at Fra Mauro (3.65° S, 342.53° E). The Apollo 14 Laser Ranging Retroreflector experiment, photographed by Cmdr. Alan Shepard. The Apollo LLR's, at Tranquility Base, Fra Mauro and a third with four times the surface area at Hadley Delta, have long been the last Apollo experiments still underway. Designed to return reflected laser light in precisely the direction from which it arrives, vastly improved lasers and detector sensitivities on Earth in the years since have allowed scientists to gauge the Earth-Moon distance with micro-precision, and tantalizing close to limits determining the "locality" of physical laws on cosmological scales [NASA/ASJ].

Joel Raupe
Lunar Pioneer

The Apollo 12 lunar landing of November 1969, in walking distance from Surveyor 3, demonstrated accumulated levels of understanding of the Moon, lunar navigation and vehicle capability that was truly stunning. Some hold the engineering accomplishment to be as great a Cold War victory as the first landing clearly was four months earlier. Like so many other unexpected discoveries in space exploration, however, new lessons and wisdom took on a greater importance with the passing of time.

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."
An article in New Scientist February 15 takes up the story now, illustrating better also why measuring the distance from Earth to the Moon, and the retroreflectors left behind on the Moon have lately taken on a new importance to cosmologists.

Recommended Article in New Scientist, HERE.

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.

Read the detailed story, HERE.



Apollo 14 at the beginning of Edgar Mitchell and Alan Shepard's first EVA in February, 1971. Erik van Meijgaarden has combined A14-9254 and 9255 as a 4 o'clock portrait of the Lunar Module, now a feature of the Apollo 14 section of the Apollo Surface Journal.

Friday, October 9, 2009

Making an Impact (40 years ago)



Smack! - A very fresh lunar crater, from the impact of Apollo 14's 3rd Stage Saturn IVB booster, intentionally impacted into the Moon, February 4, 1971 to probe the interior structure of the Moon using seismometers left by Apollo 12. [NASA/GSFC/Arizona State University].

Mark Robinson
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?


Apollo 14 S-IVB (S-IVB-509) was 17.8 m tall, 6.6 m in diameter, weighing ~14,000 kg. Launched carrying Apollo 14, January 31, 1971, after extraction of Lunar Module, remaining fuel was dumped and it was directed to impact the Moon February 4. [NASA Image ]

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


The Lunar Reconnaissance Orbiter (LRO) has returned its first imagery of the Apollo moon landing sites. The pictures show Apollo lunar module descent stages from five of the six successful manned landing site resting on the moon's surface, as long shadows from a low sunset phase angle make the modules' locations distinct.

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."

NASA Science News Release HERE.