In 1964, at least two companies were working under contract to JPL on a Surveyor Lunar Roving Vehicle Study: Bendix Corporation Systems Division, and General Motors Corporation Defense Research Laboratories. This photo shows a prototype General Motors rover, one of several different approaches that were studied to determine their capabilities, limitations, and their impact on overall spacecraft design and performance. Twelve different spacecraft configurations were studied in detail, with variations in weight, power systems, communication method, and spaceframe size.
The final design of the Surveyor 1 through 7 lunar landers did not include a rover. NASA sponsored other lunar rover studies during the 1960s, with a variety of sizes and technical capabilities, and Apollo 15 astronauts became the first to drive a Lunar Roving Vehicle on the moon, during their 1971 mission. JPL continued to develop robotic spacecraft and rovers and, in 1997, landed Mars Pathfinder and its Sojourner rover on the red planet.
In addition to the awesome views they offer, lunar eclipses have always provided scientific clues about the moon's shape, location and even surface composition. Although there will continue to be opportunities for observers to examine and reflect on fundamental concepts about the moon, such as its origin and interior structure, more modern tools are aiding these observations.
When it comes to understanding what a moon or a planet is made of remotely -- short of touching it or placing seismometers on its surface or probes below the surface -- classical physics comes to the rescue. By measuring the magnetic and gravitational forces that are generated on the inside and manifested on the outside of a planet or moon, we can learn volumes about the structure of its interior.
A spacecraft in the proximity of the moon can detect these forces. In the case of gravity, the mass of the moon will pull on the spacecraft due to gravitational attraction. If the spacecraft is transmitting a stable radio signal at the time, its frequency will shift by an amount exactly proportional to the forces pulling on the spacecraft.
This is how we weigh the moon and go further by measuring the detailed distribution of the densities of mountains and valleys as well as features below the moon's surface. This collection of information is called the gravity field.
In the past, this has lead to the discovery mascons on the moon, or hidden, sub-surface concentrations of mass not obvious in images or topography. If not accounted for, mascons can complicate the navigation of future landed missions. A mission, human or robotic, attempting to land on the moon would need to have a detailed knowledge of the gravity field in order to navigate the landing process safely. If a spacecraft sensed gravitational pull higher than planned, it could jeopardize the mission.
The Gravity Recovery and Interior Laboratory (GRAIL) mission, scheduled to launch in September, is comprised of twin spacecraft flying in formation with radio links between them to measure the moon's gravity field globally. This is because a single spacecraft with a link to Earth would be obstructed when the spacecraft goes behind the moon, leaving us with no measurement for nearly half of the moon, since the moon's far side never faces the Earth. The GRAIL technique may also reveal if the Moon has a core with a fluid layer.
So as you go out to watch the lunar eclipse on the night of Dec. 20, think about how much we've learned about the moon so far and what more we can learn through missions like GRAIL. Even at a close distance from Earth, the moon remains a mystery waiting be uncovered.
Phew! We made it through the deepest swoop yet down into the plume of Enceladus, the encounter we call "E7" because it's the seventh targeted flyby of Enceladus. But now we have our work cut out for the next few weeks as we pore over the data, painstakingly analyzing every signal to understand the composition of the plume and its structure.
So far, we know the Visual and Infrared Mapping Spectrometer (VIMS) was able to get images and data in a variety of wavelengths of light and saw that the plume extends out to at least 1,000 kilometers (600 miles).
We also have striking images of the moon crowned by its glorious plume, which Cassini captured right before its plunge. The images illustrate well that the spectacular plume spewing from the south polar region is composed of many much smaller jets.
The images and VIMS data both show that as the moon becomes less and less illuminated by the sun (similar to when our moon approaches the phase known as "new moon"), the plume gets much brighter. These data will be valuable for understanding the detailed structure of the plume and where it connects to the surface.
We have also learned that the density of the plume appears to be less than half of that predicted. Still, the heart of the plume measured on this flyby was about three times denser than the sparser parts of the plume we flew through previously.
There is more good news. We will be able to do the Enceladus flyby on April 28, 2010, on the spacecraft's reaction wheels. This means we will be able to perform the Radio Science Subsystem experiment with Cassini's main antenna to understand the interior of Enceladus under the hot south polar region.
During this experiment, antennas from the Deep Space Network (DSN) on Earth will be tracking the spacecraft to see how much Enceladus tugs on it. By measuring this tug, scientists will be able to answer such questions as: How much is the shape of the moon deformed by tidal forces from Saturn? Is there an unusually dense mass under the south pole? (The higher the mass, the larger the tug?)
We know that heating by tidal forces is what drives the plumes, but we're not sure exactly how. In addition to a possible liquid subsurface ocean, Enceladus may be harboring a dense mass underneath its surface that helped to start and maintain the moon's current activity.
Just wanted to share our excitement about the reams of data we're combing through. Now, back to work!
After so many close flybys of Enceladus, we're starting to feel as if this little moon of Saturn is an old friend. But during the encounter planned for Nov. 2, 2009, we are going to get up-close and personal. Cassini is going to take its deepest dive yet into the plumes spewing out from the moon's south pole to try to learn more about their composition and density.
The spacecraft is going to approach within about 100 kilometers (62 miles) of the surface. We've been closer before (25 kilometers or 15 miles), but we've never plunged quite so deeply into the heart of the plume.
To get a better sense of our flyby, watch the animation created by my colleague Brent Buffington. This is the seventh targeted flyby of Enceladus, so we sometimes refer to it as "E7." The video starts out with our approach to Enceladus, rotating through the various instruments scanning Enceladus for data. Then at around 7:40 a.m. UTC (Coordinated Universal Time), we do our long-anticipated flyby through the plumes. The passage will be quick: traveling at about 8 kilometers per second (about 5 miles per second) - fast enough to go from Los Angeles to New York in less than 9 minutes - we'll spend only about a minute in the plume.
Then, we zoom away from the plumes and Cassini turns on an infrared instrument (red rays in the animation) to take the temperature of the south-pole fissures known as "tiger stripes" where the plumes originate. A few minutes later, Cassini uses an ultraviolet instrument (purple rays in the animation) to measure the plumes against the background of the peach-colored Saturn. The infrared instrument then gets another turn to examine Enceladus. For more details, see the mission description.
The focus of this flyby is to analyze the particles in the plume with instruments that can detect the size, mass, charge, speed and composition. Instead of using its eyes (the cameras), Cassini is going to use its senses of taste and smell. But we're going to get some pretty good pictures too, including some impressive shots of the plumes from far away.
So far, we have detected water vapor, sodium and organic chemicals such as carbon dioxide in the plumes that spew out from the tiger stripes, but we need more detail. Are there just simple organic molecules, or something more complex? This is the first time we've found activity on a moon this small (the width of Arizona, 500 kilometers or 310 miles in diameter). We really want to understand what's driving the plumes, especially whether there is liquid water underneath the surface. If we can put the pieces together - a liquid ocean under the surface, heat driving the geysers and the organic molecules that are the building blocks of life - Enceladus might turn out to have the conditions that led to the origin of life on an earlier version of Earth.
So if this is all so interesting, why did we wait so long to travel into the plumes? One reason is the plunge is tricky. We wanted to make sure we could do it. We worried that plume particles might damage the spacecraft. We did extensive studies to determine that it was safe at these distances. We also wanted to have the right trajectory so we didn't use an excessive amount of rocket fuel. We are going very fast through this sparse plume; so to play it safe, we're using Cassini's thrusters to keep it stable through this flyby.
We'll be monitoring the thrusters closely because we don't want to have to use them on another flyby through the plumes planned for April 28, 2010. In the future flyby, we plan on tracking the spacecraft very closely with the radio instruments on Cassini and on Earth so we can measure how the spacecraft wobbles as it passes near Enceladus. These measurements should tell us more about the interior of the moon, including whether it really does have a liquid subsurface ocean. With the thrusters on, we won't be able tell if the motion of the spacecraft comes from the gravity of Enceladus or the thrusters. We'd like to know whether we can rely on other kinds of attitude control equipment.
We're all eager to pore over the results of this flyby. Stay tuned. In the meantime, feast your eyes on this map of the surface of Enceladus that the Cassini imaging team has updated and released today. The tiger stripes are located in the lower middle left and lower middle right of the image.
It's an exciting time in Cassini-land these days! We are well into the Equinox Mission, an extension to Cassini's mission that includes seven flybys of the Saturnian moon Enceladus, discovered in July 2005 to be geologically active. Prior to the prime mission, we knew that Enceladus was interesting and unique, and thus planned and executed three targeted flybys for the prime mission. With the tremendous discovery of water plumes at the south pole of this small icy moon (which happened on the second targeted flyby), we planned a more in-depth investigation for the Equinox Mission. And we are well into it! Our first Enceladus flyby of the Equinox Mission was in August, and we had two in October.
My job on Cassini is two-fold: I am on the science planning team, helping to plan out the science activities that occur during each icy moon encounter, and I am on the team for the ultraviolet imaging spectrograph instrument, studying ultraviolet data of the surfaces of these icy moons. So it’s really fantastic to be involved in planning each encounter, and then analyzing data to understand the moons.
In order to learn as much as we can about crazy Enceladus (it's so small and icy -- yet it's got these geysers!), we want to let all of the instruments make measurements, and it isn't possible to simultaneously get measurements from all instruments. (That's just the way the spacecraft is built.) We know that the cameras will tell us a lot about the current and historical geology of the surface, the ultraviolet and infrared imagers will tell us about the surface composition, and the long-wavelength infrared instrument will reveal surface temperatures. These four "remote-sensing" instruments can take data simultaneously. But if we want to get the best data from the "in situ" instruments (like the ion and neutral mass spectrometer and cosmic dust analyzer), we need to orient the spacecraft such that it's nearly impossible to get remote sensing data. So we divide up the flybys and allow many instruments the opportunity to get data. The period around the closest approach during the August flyby (called "E4") was allocated to the remote-sensing instruments -- and this resulted in the highest-resolution images of the active "tiger stripes" ever! (See one of these images here: http://photojournal.jpl.nasa.gov/catalog/PIA11113) The closest approach of the next Enceladus flyby - called "E5," on October 9 -- took the spacecraft deeper into the south polar plume than ever before. Here the priority was given to the in situ instruments, which obtained great, high-signal data of the plume, telling us about the composition of both the gaseous and particle components. And the October 31 flyby - called "E6" -- was again dedicated to remote-sensing, for a last look at the south pole before it heads mostly into seasonal darkness.
It’s so fortunate that Cassini has multiple opportunities to execute close encounters of an object as dynamic as Enceladus. The Voyager spacecraft had just one shot as they flew through the Saturn system, but Cassini, as an orbiter, gives us the chance to analyze our data, figure out what we’ve learned, and make thoughtful decisions on what experiments we need to make to follow up on those discoveries.
Things aren’t completely within our control, however! For instance, southern summer in the Saturn system is coming to a close, limiting the amount of sunlight illuminating the fascinating south polar region of Enceladus. But there’s plenty of important science to do in the dark with the in situ instruments, as well as the composite infrared spectrometer and radar, which is great. Who knows — we’ll see what the equinox season (and hopefully the following solstice) has in store for us! We may get some surprises!