In the 1970s and 80s, before advanced computer graphics, artist Ken Hodges was hired by JPL to create paintings that depicted many different missions – some in the planning stages and some only imagined.
Bruce Murray became JPL's Director in 1976, and he advocated new missions (Purple Pigeons) that would have enough pizzazz to attract public and scientific support. Hodges painted many of the Purple Pigeon images, including this scene of a Saturn orbiter with a lander going to the surface of Saturn's largest moon Titan. This artwork was done almost 30 years before Cassini's Huygens Probe reached the surface of Titan. Cassini was launched in 1997 and spent seven years traveling to Saturn. The probe was released in December 2004, and landed on Titan on January 14, 2005.
For more information about the history of JPL, contact the JPL Archives for assistance. [Archival and other sources: P-numbered photo albums and indexes, Cassini and Huygens web pages.]
Dear Pedawntic Readers,
A sophisticated spaceship in orbit around an alien world has been firing its advanced ion engine to execute complex and elegant orbital acrobatics.
On assignment from Earth at dwarf planet Ceres, Dawn is performing like the ace flier that it is.
The spacecraft’s activities are part of an ambitious bonus goal the team has recently devised for the extended mission. Dawn will maneuver to a location exactly on the line connecting Ceres and the sun and take pictures and spectra there. Measuring the opposition surge we explained last month will help scientists gain insight into the microscopic nature of the famous bright material in Occator Crater. Flying to that special position and acquiring the pictures and spectra will consume most of the rest of the extended mission, which concludes on June 30.
This month, we will look at the probe’s intricate maneuvers. Next month, we will delve more into the opposition surge itself, and in April we will describe Dawn’s detailed plans for photography and spectroscopy. In May we will discuss further maneuvers that could provide a backup opportunity for observing the opposition surge in June.
First, however, it is worth recalling that this is not Dawn’s primary responsibility, which is to continue to measure cosmic rays in order to improve scientists’ ability to establish the atomic species down to about a yard (meter) underground. Sensing the space radiation requires the spacecraft to stay more than 4,500 miles (7,200 kilometers) above the dwarf planet that is its gravitational master. The gamma ray and neutron detector will be operated continuously as Dawn changes its orbit and then performs the new observations. The ongoing high-priority radiation measurements will not be affected by the new plans.
The principal objective of the orbital maneuvers is to swivel Dawn’s orbit around Ceres. Imagine looking down on Ceres’ north pole, with the sun far to the left. (To help your imagination, you might refer to this figure from last month. As we will explain in May, Dawn’s orbital plane is slowly rotating clockwise, according to plan, and it is now even closer to vertical than depicted in January. That does not affect the following discussion.) From your perspective, looking edge-on at Dawn’s orbit, its elliptical path looks like a line, just as does a coin seen from the edge. In its current orbit (labeled 6 in that figure), Dawn moves from the bottom to the top over the north pole. When it is over the south pole, on the other side of the orbit, it flies from the top of the figure back to the bottom. The purpose of the current maneuvering is to make Dawn travel instead from the left to the right over the north pole (and from the right to the left over the south pole). This is equivalent to rotating the plane of the orbit around the axis that extends through Ceres’ poles and up to Dawn’s altitude. From the sun’s perspective, Dawn starts by revolving counterclockwise and the orbit is face-on. We want to turn it so it is edge-on to the sun.
That may not sound very difficult. After all, it amounts mostly to turning right at the north pole or left at the south pole. Spaceships in science fiction do that all the time (although sometimes they turn right at the south pole). However, it turns out to be extremely difficult in reality, not to mention lacking the cool sounds. When going over the south pole, from the top of the figure to the bottom, the spacecraft has momentum in that direction. To turn, it needs to cancel that out and then develop momentum to the left. That requires a great deal of work. It is energetically expensive. Fortunately, the ever-resourceful flight team has an affordable way.
As we discuss this more, we will present three diagrams of the trajectory. It may be challenging to follow Dawn’s three-dimensional motion on two-dimensional figures, especially if you are not accustomed to reading such depictions. Don’t worry! The team has it all under control, and it works. But consider that however complicated the figures seem, designing and flying the maneuvers is somewhat more complicated. Nevertheless, if you want to try, it might help to try to reproduce Dawn’s movements with your finger as you read the text and study the illustrations. (And if the figures are not helpful for understanding the trajectory, they may at least serve as fun optical illusions, as they did for one member of the test audience.)
Suppose you are driving from north to south and want to turn east at an intersection. You have to decrease your southward (forward) velocity somehow; otherwise, you will continue moving in that direction. You also have to increase your eastward (left) velocity, which initially is zero. That means putting on the brakes and then turning the wheel and reaccelerating, which takes work. (If you’re a stunt driver in the movies, it also may mean making smoke come out near the tires.) With your car, there are two major forces at work: the engine and the friction between the wheels and the road. For a spacecraft, the forces available are the propulsion system and the gravity of other bodies (like moons). Ceres’ only moon is Dawn itself, and there are no other helpful gravitational forces, so it’s all up to the probe’s ion engine.
Dawn was not built to perform these new maneuvers. The main tank and the xenon propellant loaded in it shortly before the spacecraft launched from Cape Canaveral did not account for such an addition to the interplanetary itinerary. The plan was to travel from Earth past Mars to Vesta, enter orbit and maneuver around the protoplanet, then break out of orbit and travel to Ceres, slip into orbit, and maneuver there. Dawn has now done all that with great distinction and already moved around more while orbiting Ceres than originally planned. Indeed, the mission has accomplished far, far more propulsive flight than any other, but now its xenon supply is very low. Navigators needed an efficient way to swivel the spacecraft’s orbit, and that meant finding an efficient way to change the direction of its orbital motion.
An orbit is the perfect balance between the inward tug of gravity and the fundamental tendency of free objects to travel in a straight line. Orbital velocity thus depends on the strength of the gravitational pull. At low altitude, orbiting objects travel faster than at higher altitude. (We have considered this topic in some detail, including with examples, several times before.) Dawn is flying to a very high altitude, where Ceres’ grip will not be as strong so the orbital velocity will naturally be much lower and therefore easier to change. Then it will turn left and swoop back down for the photo op. Any hotshot spaceship pilot would be proud to fly the same profile.
In December 2016, Dawn reached extended mission orbit 3 (XMO3), which ranged in altitude between 4,670 miles (7,520 kilometers) and 5,810 miles (9,350 kilometers). Now the spacecraft is climbing, and it will peak at more than 32,000 miles (52,000 kilometers) in early April when it will pivot the orbit almost 90 degrees. It will then glide down to about 12,400 miles (20,000 kilometers) for the targeted observations.
The maneuvering will be conducted in four stages. The first part of the ion powered ascent was Feb. 22-26, and the next will be March 8-12 when the orbital position is optimal. Although the spacecraft will stop thrusting then at an altitude of 8,000 miles (13,000 kilometers), it will have built up so much momentum that it will continue soaring upward for almost a month as Ceres’ gravitational attraction slows its down. (Dawn uses that pull as a means of putting on the brakes to reduce the forward momentum.) A third period of thrusting on April 3-14 at the apex of its arc will accomplish the turn. Dawn will then be in an orbit that will intersect the line between Occator Crater and the sun on April 29. (After turning, Dawn allows Ceres to do the work of accelerating it, as gravity brings the ship back down.)
This complex flight plan is different from all the prior powered flight, both at Vesta and at Ceres. Most of the orbit changes have been lovely spirals, and the ship rode the gravitational currents at Vesta to shift the orbital plane by a much smaller angle than it is working on now. Some of the graceful steps in this new choreography are especially delicate and require exquisite accuracy to reach just the right final trajectory. For the first time in almost two years, the spacecraft will need to take pictures of Ceres for the express purpose of helping navigators plot its progress. (In the intervening time, Dawn has taken more than 55,000 photos specifically to study the dwarf planet. Many of them also have been used for navigation.) Combining these "optical navigation" pictures with their other navigational techniques, the team will design a final, fourth stage of ion thrusting for April 22-24 to fine tune the orbit. We have described such trajectory correction maneuvers before. (It’s easier for you to chart the spacecraft’s progress than it is for the Dawn team. All you have to do is read the mission status reports.)
By the time it began ion thrusting last week, Dawn had successfully completed all of its assignments in XMO3. That included three photography sessions. In the last, the spacecraft used the primary and backup cameras simultaneously for the first time in the entire mission. In its extensive investigations of Vesta and Ceres, Dawn has taken more than 85,000 pictures, but all of them had been with only one camera powered on at a time, the other being held in reserve. In April we will discuss the reason for operating differently before leaving XMO3.
Dawn’s adventure has been long and its experiences manifold. In just a few days, the bold explorer will mark its second anniversary of arriving at Ceres. (That’s the second anniversary as reckoned by inhabitants of Earth. In contrast, for locals, the immigrant from distant Earth has been in residence for less than half a Cerean year, although more than 1,900 Cerean days.) In 2011-2012, the probe spent almost 14 months in orbit around the giant protoplanet Vesta, the second largest object in the main asteroid belt. The only craft ever to orbit two alien destinations, it is a denizen of deep space. In its nearly 9.5-year solar system journey, Dawn has traveled 3.7 billion miles (6.0 billion kilometers). For most of this time, the spaceship has been in orbit around the sun, just as its erstwhile home Earth is. Now it has been in orbit around remote worlds for a third of its total time in space. And for you numerologists, March 5 will mark Dawn’s being in orbit around its targets for pi years. (Happy pi-th anniversary.)
Readers on or near Earth who appreciate following such an extraordinary extraterrestrial expedition can take advantage of an opportunity this week to do a little celestial navigation of their own. On March 2, the moon will serve as a helpful signpost to locate the faraway ship on the interplanetary seas. From our terrestrial viewpoint, the moon will move very close to Dawn’s location in the sky. The specifics, of course, depend on your exact location. For many afternoon sky watchers in North America, the moon will come to within about a degree, or two lunar diameters, of Dawn. As viewed by some observers in South America, the moon will pass directly in front of Dawn. For most Earthlings, when the moon rises on the morning of March 2, it will be north and east of Dawn. During the day, the moon will gradually drift closer and, from many locations, pass the spacecraft and the dwarf planet it orbits. The angle separating them will be less than the width of your palm at arm’s length, providing a handy way to find our planet’s emissary. Although Dawn and Ceres will appear to be near the moon, they will not be close to it at all. The distant spacecraft will be more than 1,300 times farther away than the moon by then (and well over one million times farther than the International Space Station) and quite invisible. But your correspondent invites you to gaze in that direction as you raise a saluting hand to humankind’s insatiable appetite for knowledge, irresistible drive for exploration, passion for adventure, and longing to know the cosmos.
Dawn is 7,300 miles (11,800 kilometers) from Ceres. It is also 3.19 AU (296 million miles, or 477 million kilometers) from Earth, or 1,280 times as far as the moon and 3.22 times as far as the sun today. Radio signals, traveling at the universal limit of the speed of light, take 53 minutes to make the round trip.
Dr. Marc D. Rayman
4:30 p.m. PST February 27, 2017
In early 1989, a series of thermal tests were conducted on the Microwave Limb Sounder (MLS) Instrument, which was part of the Upper Atmosphere Research Satellite (UARS).
The MLS System Thermal Vacuum (STV) test program was designed to evaluate its thermal integrity and functions in a simulated space environment. It included a 24-hour bakeout, six phases of thermal balance tests, and a thermal cycling test of the instrument in flight configuration, using a variety of heaters and lamps.
This photo shows the Ten-Foot Space Simulator located in Building 248, with a quartz lamp array approximately seven feet tall. This array faced the primary reflector during testing and helped to heat the chamber to 80°C (176°F). The vacuum chamber shroud was lowered over the test fixture, and the chamber walls and floor were maintained at -100°C to -179°C during testing.
For more information about the history of JPL, contact the JPL Archives for assistance.
“This year we’re gonna bring it!”
Oceans Melting Greenland (OMG) Principal Investigator Josh Willis told me excitedly. “It’s the beginning of year two of this five-year airborne mission, which means that by comparing data from the first and second years, we’ll be able to observe changes in Greenland’s glaciers and coastal ocean water for the first time.” Glaciers around Greenland’s jagged coastline have been melting into the ocean and causing increased sea level rise, so measuring the amount of ice mass loss will help us understand the impact of these changes, Willis said. “Will we see 5 feet of sea level rise this century … or more?”
See, Earth’s ocean, more than the atmosphere, is responsible for creating a stable climate. And as global warming has increased the temperature of the ocean waters surrounding Greenland, that warmer ocean water is melting the ice sheet from around its edges. “Hey! The ocean is eating away at the ice sheet!” Willis often cries when explaining the mission. And Team OMG is measuring how much of that warm water could be increasing due to climate change.
Decoding the environment
I understand how Willis and Project Manager Steve Dinardo get excited about measuring sea level rise. Greenland’s ice melt is accelerating, which explains why NASA is paying attention to it. Plus, after a successful first year, the team is fully aware of the stark beauty of Greenland’s rugged landscape and seascape and the rewards of bonding as a team. Dinardo told me he was “ecstatic about the incredible progress Team OMG has made in the last twenty-two months.”
As scientists, decoding the natural world is our way of caring about the environment. We care about Greenland’s icy coastline, so we go there. We go there and observe. We go there and measure. For there is something undeniable about the sheer beauty of this planet, and any time you get to experience it is a moment to feel exuberant and alive. Plus, flying around with a great team in a modified NASA G-III aircraft ain’t too shabby either.After a successful first year, the team is fully aware of the stark beauty of Greenland’s rugged landscape and seascape and the rewards of bonding as a team.
But wait. Before I continue, there’s something you probably noticed: Willis said he named this Greenland observing expedition Oceans Melting Greenland, or OMG for short, because, hey, OMG is the exact response you might have when you find out what’s going on up there.
Parts of Greenland’s coastline are so remote, so difficult to access by boat, that they’d remain uncharted, especially under areas that are seasonally covered with ice. Imagine the edge of an unimaginably complicated winding coastline, that unknown place where ice meets water meets seafloor. Big chunks of remnant sea ice clog up the water, and the glacier has retreated so recently that the coastline is changing as fast as, or even faster than, we can study it.
The seawater around 400 meters deep is 3 to 4 degrees Celsius warmer than the water floating near the sea surface. And the sea floor bathymetry influences how much of that warm subsurface layer can reach far up into the fjords and melt the glaciers. So, to learn about the interface between where the bottom of the ice sheet reaches out over the seawater and down into the ocean, OMG began by mapping undersea canyons on the M/V Cape Race, a ship equipped with an echo sounder, which sailed right up the narrow fjords on the continental shelf surrounding Greenland to the places where the warmer Atlantic Ocean water meets the bottoms of the frozen, 0-degree glaciers. The crew had to snake in between floating icebergs and weave in and out of narrow fjords. The Cape Race used a multibeam echo sounder to map undersea canyons, where the warm seawater comes in contact with and melts the glaciers.
The next four years
In the spring of 2016, the Oceans Melting Greenland (OMG) team began surveying glacier elevation near the end of marine-terminating glaciers by precisely measuring the edges of the ice sheet on a glacier-by-glacier basis, using the Airborne Glacier and Land Ice Surface Topography Interferometer (GLISTIN-A), a radar instrument attached to the bottom of a modified NASA G-III aircraft. Data collected this spring and over the next four years can be compared with data collected in the spring of 2016 so we can determine how fast the glaciers are melting.
The investigation continued into last fall, with the team dropping more than 200 Aircraft eXpendable Conductivity Temperature Depth (AXCTD) probes that measured ocean temperature and salinity around Greenland, from the sea surface to the sea floor, through a hole in the bottom of the plane. “In most of these places,” Willis told me, “there’s been no temperature and salinity data collected. Ever.”As scientists, decoding the natural world is our way of caring about the environment.
The team will drop more ocean probes across the same locations to find out “how much ice melts when the water is this warm,” what the melt rate is, and how much that rate is increasing, because no one knows the melt rate yet.
Big picture project
“OMG is a big picture project,” Willis explained. ”We want to see what’s happening in the ocean on the large scale and what’s happening to the ice sheet on the largest scales.”
As part of Team OMG, I also flew on NASA’s G-III into uncontrolled airspace to places where no other aircraft had flown before, into narrow and steep ice-covered fjords, winding in and out, up and down, over and through to observe and measure, like scientists do. I saw the brilliant white ice carve its way through steep brown valleys into open ocean water. I saw the glorious expanse of white upon deep blue going on and on and on below us as we flew just 5,000 feet above the winding coastline. It was extraordinary.
And if you just thought “OMG,” Willis would be proud.
Thanks for reading.
A deep-space robotic emissary from Earth is continuing to carry out its extraordinary mission at a distant dwarf planet.
Orbiting high above Ceres, the sophisticated Dawn spacecraft is hard at work unveiling the secrets of the exotic alien world that has been its home for almost two years.
Dawn’s primary objective in this sixth orbital phase at Ceres (known as extended mission orbit 3, XMO3 or "this sixth orbital phase at Ceres") is to record cosmic rays. Doing so will allow scientists to remove that "noise" from the nuclear radiation measurements performed during the eight months Dawn operated in a low, tight orbit around Ceres. The result will be a cleaner signal, revealing even more about the atomic constituents down to about a yard (meter) underground. As we will see below, in addition to this ongoing investigation, soon the adventurer will begin pursuing a new objective in its exploration of Ceres.
With its uniquely capable ion propulsion system, Dawn has flown to orbits with widely varying characteristics. In contrast to the previous five observation orbits (and all the observation orbits at Vesta), XMO3 is elliptical. Over the course of almost eight days, the spacecraft sails from a height of about 4,670 miles (7,520 kilometers) up to almost 5,810 miles (9,350 kilometers) and back down. Dutifully following principles discovered by Johannes Kepler at the beginning of the 17th century and explained by Isaac Newton at the end of that century, Dawn’s speed over this range of altitudes varies from 210 mph (330 kilometers per hour) when it is closest to Ceres to 170 mph (270 kilometers per hour) when it is farthest. Yesterday afternoon, the craft was at its highest for the current orbit. During the day today, the ship will descend from 5,790 miles (9,310 kilometers) to 5,550 miles (8,930 kilometers). As it does so, Ceres’ gravity will gradually accelerate it from 170 mph (273 kilometers per hour) to 177 mph (285 kilometers per hour). (Usually we round the orbital velocity to the nearest multiple of 10. In this case, however, to show the change during one day, the values presented are more precise.)
As we saw last month, the angle of XMO3 to the sun presents an opportunity to gain a new perspective on Ceres, with sunlight coming from a different angle. (We include the same figure here, because we will refer to it more below.) Last week, Dawn took advantage of that opportunity, seeing the alien landscapes in a new light as it took pictures for the first time since October.
Dawn takes more than a week to revolve around Ceres, but Ceres turns on its axis in just nine hours. Because Dawn moves through only a small segment of its orbit in one Cerean day, it is almost as if the spacecraft hovers in place as the dwarf planet pirouettes beneath it. During one such period on Jan. 27, Dawn’s high perch moved only from 11°N to 12°S latitude as Ceres presented her full range of longitudes to the explorer’s watchful eye. This made it very convenient to take pictures and visible spectra as the scenery helpfully paraded by. (The spacecraft was high enough to see much farther north and south than the latitudes immediately beneath it.) Dawn will make similar observations again twice in February.
As Dawn was expertly executing the elegant, complex spiral ascent from XMO2 to XMO3 in November, the flight team considered it to be the final choreography in the venerable probe’s multi-act grand interplanetary performance. By then, Dawn had already far exceeded all of its original objectives at Vesta and Ceres, and the last of the new scientific goals could be met in XMO3, the end of the encore. The primary consideration was to keep Dawn high enough to measure cosmic rays, meaning it needed to stay above about 4,500 miles (7,200 kilometers). There was no justification or motivation to go anywhere else. Well, that’s the way it was in November anyway. This is January. And now it’s (almost) time for a previously unanticipated new act, XMO4.
Always looking for ways to squeeze as much out of the mission as possible, the team has now devised a new and challenging investigation. It will consume the next five months (and much of the next five Dawn Journals). We begin this month with an overview, but follow along each month as we present the full story, including a detailed explanation of the underlying science, the observations themselves and the remarkable orbital maneuvering entirely unlike anything Dawn has done before. (You can also follow along with your correspondent’s uncharacteristically brief and more frequent mission status updates.)
From the XMO3 vantage point, with sunlight coming from the side, Ceres is gibbous and looks closer to a half moon than full. The new objective is to peer at Ceres when the sun is directly behind Dawn. This would be the same as looking at a full moon. (In the figure above, it would be like photographing Ceres from somewhere on the dashed line that points to the distant sun.)
While Dawn obtained pictures from near the line to the sun in its first Ceres orbit, there is a special importance to being even closer to that line. Let’s see why that alignment is valuable.
Most materials reflect light differently at different angles. You can investigate this yourself (and it’s probably easier to do at home than it is in orbit around a remote dwarf planet). To make it simpler, take some object that is relatively uniform (but with a matte finish, not a mirror-like finish) and vary the angles at which light hits it and from which you look at it. You may see that it appears dimmer or brighter as the angles change. It turns out that this effect may be used to help infer the nature of the reflecting material. (For the purposes of this exercise, if you can hold the angle of the object relative to your gaze fixed, and vary only the angle of the illumination, that’s best. But don’t worry about the details. Conducting this experiment represents only a small part of your final grade.)
Now when scientists carefully measure the reflected light under controlled conditions, they find that the intensity changes quite gradually over a wide range of angles. In other words, the apparent brightness of an object does not vary dramatically as the geometry changes. However, when the source of the illumination gets very close to being directly behind the observer, the reflection may become quite a bit stronger. (If you test this, of course, you have to ensure your shadow doesn’t interfere with the observation. Vampires don’t worry about this, and we’ll explain below why Dawn needn’t either.)
If you (or a helpful scientist friend of yours) measure how bright a partial moon is and then use that information to calculate how bright the full moon will be, you will wind up with an answer that’s too small. The full moon is significantly brighter than would be expected based on how lunar soil reflects light at other angles. (Of course, you will have to account for the fact that there is more illuminated area on a full moon, but this curious optical behavior is different. Here we are describing how the brightness of any given patch of ground changes.)
A full moon occurs when the moon and sun are in opposite directions from Earth’s perspective. That alignment is known as opposition. That is, an astronomical body (like the moon or a planet) is in opposition when the observer (you) is right in between it and the source of illumination (the sun), so all three are on a straight line. And because the brightness takes such a steep and unexpected jump there, this phenomenon is known as the opposition surge.
The observed magnitude of the opposition surge can reveal some of the nature of the illuminated object on much, much finer scales than are visible in photos. Knowing the degree to which the reflection strengthens at very small angles allows scientists to ascertain (or, at least, constrain) the texture of materials on planetary surfaces even at the microscopic level. If they are fortunate enough to have measurements of the reflectivity at different angles for a region on an airless solar system body (atmospheres complicate it too much), they compare them with laboratory measurements on candidate materials to determine which ones give the best match for the properties.
Dawn has already measured the light reflected over a wide range of angles, as is clear from the figure above showing the orbits. But the strongest discrimination among different textures relies on measuring the opposition surge. That is Dawn’s next objective, a bonus in the bonus extended mission.
You can see from the diagram that measuring the opposition surge will require a very large change in the plane of Dawn’s orbit. Shifting the plane of a spacecraft’s orbit can be energetically very, very expensive. (We will discuss this more next month.) Fortunately, the combination of the unique capabilities provided by the ion propulsion system and the ever-creative team makes it affordable.
Powered by an insatiable appetite for new knowledge, Dawn will begin ion thrusting on Feb. 23. After very complex maneuvers, it will be rewarded at the end of April with a view of a full Ceres from an altitude of around 12,400 miles (20,000 kilometers), about the height of GPS satellites above Earth. (That will be about 50 percent higher than the first science orbit, which is labeled as line 1 in the figure.) There are many daunting challenges in reaching XMO4 and measuring the opposition surge. Even though it is a recently added bonus, and the success of the extended mission does not depend on it, mission planners have already designed a backup opportunity in case the first attempt does not yield the desired data. The second window is late in June, allowing the spacecraft time to transmit its findings to Earth before the extended mission concludes at the end of that month.
For technical reasons, the measurements need to be made from a high altitude, and throughout the complex maneuvering to get there, Dawn will remain high enough to monitor cosmic rays. Ceres will appear to be around five times the width of the full moon we see from Earth. It will be about 500 pixels in diameter in Dawn’s camera, and more than 180,000 pixels will show light reflected from the ground. Of greatest scientific interest in the photographs will be just a handful of pixels that show the famous bright material in Occator Crater, known as Cerealia Facula and clearly visible in the picture above. Scientists will observe how those pixels surge in brightness over a narrow range of angles as Dawn’s XMO4 orbital motion takes it into opposition, exactly between Occator and the sun. Of course, the pictures also will provide information on how the widespread dark material covering most of the ground everywhere else on Ceres changes in brightness (or, if you prefer, in dimness). But the big reward here would be insight into the details of Cerealia Facula. Comparing the opposition surges with laboratory measurements may reveal characteristics that cannot be discerned any other way save direct sampling, which is far beyond Dawn’s capability (and authority). For example, scientists may be able to estimate the size of the salt crystals that make up the bright material, and that would help establish their geological history, including whether they formed underground or on the surface. We will discuss this more in March.
Most of the data on opposition surges on solar system objects use terrestrial observations, with astronomers waiting until Earth and the target happen to move into the necessary alignment with the sun. In those cases, the surge is averaged over the entire body, because the target is usually too far away to discern any details. Therefore, it is very difficult to learn about specific features when observing from near Earth. Few spacecraft have actively maneuvered to acquire such data because, as we alluded to above and will see next month, it is too difficult, especially at a massive body like Ceres. The recognition that Dawn might be able to complete this challenging measurement for a region of particular interest represents an important possibility for the mission to discover more about this intriguing dwarf planet’s geology.
Meeting the scientific goal will require a careful and quantitative analysis of the pixels, but the images of a fully illuminated Ceres will be visually appealing as well. Nevertheless, you are cautioned to avoid developing a mistaken notion about the view. (For that matter, you are cautioned to avoid developing mistaken notions about anything.) You might think (and some readers wondered about this in a different phase of the mission) that with Dawn being between the sun and Ceres (and not being a vampire), the spacecraft’s shadow might be visible in the pictures. It would look really cool if it were (although it also would interfere with the measurement of the opposition surge by introducing another factor into how the brightness changes). There will be no shadow. The spacecraft will simply be too high. Imagine you’re standing in Occator Crater, either wearing your spacesuit while engaged in a thrilling exploration of a mysterious and captivating extraterrestrial site or perhaps instead while you’re indoors enjoying some of the colony’s specially salted Cerean savory snacks, famous throughout the solar system. In any case, the distant sun you see would be a little more than one-third the size that it looks from Earth, comparable to a soccer ball at 213 feet (65 meters). Dawn would be 12,400 miles (20,000 kilometers) overhead. Although it’s one of the largest interplanetary spacecraft ever to take flight, with a wingspan of 65 feet (20 meters), it would be much too small for you to see at all without a telescope and would block an undetectably small amount of sunlight. It would appear smaller than a soccer ball seen from 135 miles (220 kilometers). Therefore, no shadow will be cast, the measurement will not be compromised by the spacecraft blocking some of the light reaching the ground and the pictures will not display any evidence of the photographer.
Even as the team was formulating plans for this ambitious new campaign, they successfully dealt with a glitch on the spacecraft this month. When a routine communications session with the Deep Space Network began on Jan. 17, controllers discovered that Dawn had previously entered its safe mode, a standard response the craft uses when it encounters conditions its programming and logic cannot accommodate. The main computer issues instructions to reconfigure systems, broadcasts a special radio signal through one of the antennas and then patiently awaits help from humans on a faraway planet (or anyone else who happens to lend assistance). The team soon determined what had occurred. Since it left Earth, Dawn has performed calculations five times per second about its location and speed in the solar system, whether in orbit around the sun, Vesta or Ceres. (Perhaps you do the same on your deep-space voyages.) However, it ran into difficulty in those calculations on Jan. 14 for the first time in more than nine years of interplanetary travel. To ensure the problematic calculations did not cause the ship to take any unsafe actions, it put itself into safe mode. Engineers have confirmed that the problem was in software, not hardware and not even a cosmic ray strike, which has occasionally triggered safe mode, most recently in September 2014.
Mission controllers guided the spacecraft out of safe mode within two days and finished returning all systems to their standard configurations shortly thereafter. Dawn was shipshape the subsequent week and resumed its scientific duties. When it activated safe mode, the computer correctly powered off the gamma ray and neutron detector, which had been measuring the cosmic rays, as we described above. The time that the instrument was off will be inconsequential, however, because there is more than enough time in the extended mission to acquire all the desired measurements.
The extended mission has already proven to be extremely productive, yielding a great deal of new data on this ancient world. But there is still more to look forward to as the veteran explorer prepares for a new and adventurous phase of its extraordinary extraterrestrial expedition.
Dawn is 5,650 miles (9,100 kilometers) from Ceres. It is also 2.87 AU (266 million miles, or 429 million kilometers) from Earth, or 1,135 times as far as the moon and 2.91 times as far as the sun today. Radio signals, traveling at the universal limit of the speed of light, take 48 minutes to make the round trip.
Dawn is concluding a remarkable year of exploring dwarf planet Ceres. At the beginning of 2016, the spacecraft was still a newcomer to its lowest altitude orbit (the fourth since arriving at Ceres in March 2015), and the flight team was looking forward to about three months of exciting work there to uncover more of the alien world’s mysteries.
As it turned out, Dawn spent more than eight months conducting an exceptionally rewarding campaign of photography and other investigations, providing a richly detailed, comprehensive look at the extraterrestrial landscapes and garnering an extraordinary bounty of data. In September, the craft took advantage of its advanced ion propulsion system to fly to a new orbit from which it performed still more unique observations in October. Last month, the ship took flight again, and now it is concluding 2016 in its sixth science orbit.
Dawn is in an elliptical orbit, sailing from about 4,670 miles (7,520 kilometers) up to up to almost 5,810 miles (9,350 kilometers) and back down. It takes nearly eight days to complete each orbital loop. Flying this high above Ceres allows Dawn to record cosmic rays to enhance the nuclear spectra it acquired at low altitude, improving the measurements of atomic constituents down to about a yard (meter) underground.
The spacecraft has been collecting cosmic ray data continuously since reaching this orbit (known to the Dawn team, imaginative readers of last month’s Dawn Journal and now you as extended mission orbit 3, or XMO3). These measurements will continue until the end of the extended mission in June. But there is more in store for the indefatigable adventurer than monitoring space radiation.
Based on studies of Dawn’s extensive inspections of Ceres so far, scientists want to see certain sites at new angles and under different illumination conditions. Next month, Dawn will begin a new campaign of photography and visible spectroscopy. All of Dawn’s five previous science orbits had different orientations from the sun. And now XMO3 will provide another unique perspective on the dwarf planet's terrain. The figure below shows what the orientation will be when the explorer turns its gaze once again on Ceres for the first set of new observations on Jan. 27, 2017.
We mentioned in the figure caption that the alignments are simplified. One of the simplifications is that some of the orbits covered a range of angles. There is a well-understood and fully predictable natural tendency for the angle to increase. In some phases of the mission, the flight team allows that, and in others they do not, depending on what is needed for the best scientific return. At the lowest altitude (orbit 4 in the diagram, and sometimes known as LAMO, XMO1 or "the lowest orbit"), navigators held the orbit at a fixed orientation. Had they not done so, it would have changed quite dramatically over the course of the eight months Dawn was there. For XMO3, the team has decided not to keep the angle constant. Therefore, later observations will provide still different views. We will return to this topic in a few months.
We have described before how places that remain shadowed throughout the Cerean year can trap water molecules. Dawn’s pictures have revealed well over 600 craters high in the northern hemisphere that are permanently in darkness, covering more than 800 square miles (more than 2,000 square kilometers). (It has not been possible to make as thorough a census of the southern hemisphere, because it has been fall and winter there during most of Dawn’s studies, so some areas were not lit well enough. Now that spring has come, new photography will tell us more.)
Dawn peered into craters to see what was hidden on the dark floors. Long exposures could reveal hints of the scenery using the faint light reflected from crater walls. In 10 of the craters, scientists found bright deposits. In one of those craters, the reflective material extends beyond the permanent shadow and so is occasionally illuminated, albeit still with the sun very low on the horizon. And sure enough, right there, Dawn’s infrared mapping spectrometer found the characteristic fingerprint of ice. These shadowed crater floors accumulate water that happens to land there, preserving it in a deep freeze that may be colder than -260°F (-163°C). Readers are invited to formulate their own business plans for how best to utilize that precious resource.
Jan. 1 is the anniversary of the discovery of Ceres. When Giuseppe Piazzi spotted the faint smudge of light in his telescope that night in 1801, he did not know that it would be known as a planet for almost two generations. (After all, he was an astronomer and mathematician, not a clairvoyant.) And he could never have imagined that more than two centuries later (by which time Ceres was known as a dwarf planet, reflecting progress in scientific knowledge), humankind would undertake an ambitious expedition to explore it, dispatching a sophisticated ship to take up residence at that distant and mysterious place. What Piazzi discovered was a lovely jewel set against the deep blackness of space and surrounded by myriad other gleaming stellar jewels. What Dawn has discovered is a unique and fascinating world of complex geology, composed of rock and ice and salt, with exotic and beautiful scenery. And as Dawn continues to build upon Piazzi’s legacy, unveiling Ceres’ secrets, everyone who has ever looked in wonder at the night sky, everyone who has ever hungered for new understanding, everyone who has ever felt the lure of a thrilling adventure far from home and everyone who has ever yearned to know the cosmos will share in the rewards.
Dawn is 5,640 miles (9,070 kilometers) from Ceres. It is also 2.43 AU (226 million miles, or 364 million kilometers) from Earth, or 915 times as far as the moon and 2.48 times as far as the sun today. Radio signals, traveling at the universal limit of the speed of light, take 41 minutes to make the round trip.
Dr. Marc D. Rayman
4:00 p.m. PST December 29, 2016
In January 1953, JPL was in the market for its first digital computer.
After investigating the possibilities, a site visit was made to Consolidated Engineering Corporation (CEC) in Pasadena and the CEC Model 30-203 digital computer, shown in this photo, was eventually selected. The prototype at CEC was given the project number 36-101. JPL and the National Bureau of Standards were the first two customers to order the computer – the one ordered by JPL was 36-102, and the one for NBS was 36-103.
JPL's computer was finally delivered and operational in July 1954. It cost approximately $135,000 (more than $1 million in 2016 dollars). That did not include the operator's console, paper tape input and output, punch card unit, or other related equipment. It featured magnetic drum storage of about 4000 words (a "word" being a number or command) and a word length of 10 decimal digits. It contained more than 1,500 vacuum tubes.
For more information about the history of JPL, contact the JPL Archives for assistance. [Archival and other sources: Section 371 photo albums, Combined Bimonthly Summary No. 33, Datatron Chronology.)
Blue rope lights adorn Dawn mission control at JPL, but not because the flight team is in the holiday spirit (although they are in the holiday spirit).
The felicitous display is more than decorative. The illumination indicates that the interplanetary spacecraft is thrusting with one of its ion engines, which emit a lovely, soft bluish glow in the forbidding depths of space. Dawn is completing another elegant spiral around dwarf planet Ceres, maneuvering to its sixth science orbit.
Dawn’s ion propulsion system has allowed the probe to accomplish a mission unlike any other, orbiting two distant extraterrestrial destinations. Even more than that, Dawn has taken advantage of the exceptional efficiency of its ion engines to fly to orbits at different altitudes and orientations while at Vesta and at Ceres, gaining the best perspectives for its photography and other scientific investigations.
Dawn has thrust for a total of 5.7 years during its deep-space adventure. All that powered flight has imparted a change in the ship’s velocity of 25,000 mph (40,000 kilometers per hour). As we have seen, this is not the spacecraft’s actual speed, but it is a convenient measure of the effect of its propulsive work. Reaching Earth orbit requires only about 17,000 mph (less than 28,000 kilometers per hour). In fact, Dawn’s gentle ion engines have delivered almost 98 percent of the change in speed that its powerful Delta 7925H-9.5 rocket provided. With nine external rocket engines and a core consisting of a first stage, a second stage and a third stage, the Delta boosted Dawn by 25,640 mph (41,260 kilometers per hour) from Cape Canaveral out of Earth orbit and onto its interplanetary trajectory, after which the remarkable ion engines took over. No other spacecraft has accomplished such a large velocity change under its own power. (The previous record holder, Deep Space 1, achieved 9,600 mph, or 15,000 kilometers per hour.)
Early this year, we were highly confident Dawn would conclude its operational lifetime in its fourth orbit at Ceres (and remain there long after). But unexpectedly healthy and with an extension from NASA, Dawn is continuing its ambitious mission. After completing all of its tasks in its fifth scientific phase at Ceres, Dawn is pursuing new objectives by flying to another orbit for still more discoveries. Although we never anticipated adding a row to the table of Dawn’s orbits, last presented in December 2015, we now have an updated version.
in ft (m)
distance of a soccer ball
|1||RC3||04.23.15 – 05.09.15||8,400
|3||HAMO||08.17.15 – 10.23.15||915
|12.16.15 – 09.02.16||240
|5||XMO2||10.16.16 – 11.04.16||920
As with the obscure Dawn code names for other orbits, this fifth orbit’s name requires some explanation. The extended mission is devoted to undertaking activities not envisioned in the prime mission. That began with two extra months in the fourth mapping orbit performing many new observations, but because it was then the extended mission, that orbit was designated extended mission orbit 1, or XMO1. (It should have been EMO1, of course, but the team’s spellchecker was offline on July 1, the day the extended mission started.) Therefore, the next orbit was XMO2. Dawn left XMO2 on Nov. 4, and we leave it to readers’ imaginations to devise a name for the orbit the spacecraft is now maneuvering to.
Surprisingly, Dawn is flying higher to enhance part of the scientific investigation that motivated going to the lowest orbit. We have explained before that Dawn’s objective in powering its way down to the fourth mapping orbit was to make the most accurate measurements possible of gravity and of nuclear radiation emitted by the dwarf planet.
For more than eight months, the explorer orbited closer to the alien world than the International Space Station is to Earth, and the gamma ray spectra and neutron spectra it acquired are outstanding, significantly exceeding all expectations. But ever-creative scientists have recognized that even with that tremendous wealth of data, Dawn can do still better. Let’s look at this more carefully and consider an example to resolve the paradox of how going higher can yield an improvement.
The gamma ray and neutron detector (GRaND) reveals some of Ceres’ atomic constituents down to about a yard (meter) underground. The principal limitation in analyzing these spectra is "noise." In fact, noise limits the achievable accuracy of many scientific measurements. It isn’t necessarily the kind of noise that you hear from loud machinery (nor from the mouth of your unhelpful parent, inattentive progeny or boring and verbose coworker), but all natural systems have something similar. Physical processes other than the ones of interest make unwanted contributions to the measurements. The part of a measurement scientists want is called the "signal." The part of a measurement scientists don’t want is called the "noise." The quality of a measurement may be characterized by comparing the strength of the signal to the strength of the noise. (This metric is called the "signal to noise ratio" by people who like to use jargon like "signal to noise ratio.")
We have discussed that cosmic rays, radiation that pervades space, strike atomic nuclei on Ceres, creating the signals that GRaND measures. Remaining at low altitude would have allowed Dawn to enhance its measurement of the Cerean nuclear signal. But scientists determined that an even better way to improve the spectra than to increase the signal is to decrease the noise. GRaND’s noise is a result of cosmic rays impinging directly on the instrument itself and on nearby parts of the spacecraft. With a more thorough measurement of the noise from cosmic rays, scientists will be able to mathematically remove that component of the low altitude measurements, leaving a clearer signal.
For an illustration of all this, suppose you want to hear the words of a song. The words are the signal and the instruments are the noise. (This is a scientific discussion, not a musical one.) It could be that the instruments are so loud and distracting that you can’t make the words out easily.
You might try turning up the volume, because that increases the signal, but it increases the noise as well. If the performance is live, you might even try to position yourself closer to the singer, perhaps making the signal stronger without increasing the noise too much. (Other alternatives are simply to Google the song or ask the singer for a copy of the lyrics, but those methods would ruin this example.)
If you’re doing this in the 21st century (or later), there’s another trick you can employ, taking advantage of computer processing. Suppose you had a recording of the singing with the instruments and then obtained separate recordings of the instruments. You could subtract the musical sounds that constitute the noise, removing the contributions from both guitars, the drums, the harp, both ukuleles, the kazoo and all the theremins. And when you eliminate the noise of the instruments, what remains is the signal of the words, making them much more intelligible.
To obtain a better measure of the noise, Dawn needs to go to higher altitude, where GRaND will no longer detect Ceres. It will make detailed measurements of cosmic ray noise, which scientists then will subtract from their measurements at low altitude, where GRaND observed Ceres signal plus cosmic ray noise. The powerful capability to raise its orbit so much affords Dawn the valuable opportunity to gain greater insight into the atomic composition. Of course, it’s not quite that simple, but essentially this method will help Dawn hear Ceres’ nuclear song more clearly.
To travel from one orbit to another, the sophisticated explorer has followed complex spiral routes. We have discussed the nature of these trajectories quite a bit, including how the operations team designs and flies them. But now they are using a slightly different method.
Those of you at Ceres who monitor the ship’s progress probably wouldn’t notice a difference in the type of trajectory. And the rest of you on Earth and elsewhere who keep track through our mission status updates also would not detect anything unusual in the ascent profile (to the extent that a spacecraft using ion propulsion to spiral around a dwarf planet is usual). But celestial navigators are now enjoying their use of a method they whimsically call local maximal energy spiral feedback control.
The details of the new technique are not as important for our discussion here as one of the consequences: Dawn’s next orbit will not be nearly as circular as any of its other orbits at Ceres (or at Vesta). Following the conclusion of this spiral ascent on Dec. 5, navigators will refine their computations of the orbit, and we will describe the details near the end of the month. We will see that as the spacecraft follows its elliptical loops around Ceres, each taking about a week, the altitude will vary smoothly, dipping below 4,700 miles (7,600 kilometers) and going above 5,700 miles (9,200 kilometers). Such a profile meets the mission’s needs, because as long as the craft stays higher than about 4,500 miles (7,200 kilometers), it can make the planned recordings of the cacophonous cosmic rays. We will present other plans for this next phase of the mission as well, including photography, in an upcoming Dawn Journal.
As Dawn continues its work at Ceres, the dwarf planet continues its stately 4.6-year-long orbit around the sun, carrying Earth’s robotic ambassador with it. Ceres follows an elliptical path around the sun (see, for example, this discussion, including the table). In fact, all orbits, including Earth’s, are ellipses. Ceres’ orbit is more elliptical than Earth’s but not as much as some of the other planets. The shape of Ceres’ orbit is between that of Saturn (which is more circular) and Mars (which is more elliptical). (Of course, Ceres’ orbit is larger than Mars’ and smaller than Saturn’s, but here we are describing how much each orbit deviates from a perfect circle.)
When Ceres tenderly took Dawn into its gravitational embrace in March 2015, they were 2.87 AU (267 million miles, or 429 million kilometers) from the sun. In January 2016, we mentioned that Ceres had reached its aphelion, or greatest distance from the sun, at 2.98 AU (277 million miles, or 445 million kilometers). Today at 2.85 AU (265 million miles, or 427 million kilometers), Ceres is closer to the sun than at any time since Dawn arrived, and the heliocentric distance will gradually decrease further throughout the extended mission. (If the number of numbers is overwhelming here, you might reread this paragraph while paying attention to only one set of units, whether you choose AU, miles or kilometers. Ignore the other two scales so you can focus on the relative distances.)
Another consequence of orbiting the sun is the progression of seasons. Right on schedule, as we boldly predicted in August 2015, Nov. 13 was the equinox on Ceres, marking the beginning of northern hemisphere autumn and southern hemisphere spring. Although it is celebrated on Ceres with less zeal than on Earth, it is fundamentally the same: the sun was directly over the equator that day, and now it is moving farther south. It takes Ceres so long to orbit the sun that this season will last until Dec. 22, 2017.
A celebration that might occur on Ceres (and which you, loyal Dawnophile, are welcome to attend) would honor Dawn itself. Although the spacecraft completed its ninth terrestrial year of spaceflight in September, on Dec. 12, it will have been two Cerean years since Dawn left Earth for its interplanetary journey. Be sure to attend in order to learn how a dawnniversary is commemorated in that part of the solar system.
Although a year on Ceres lasts much longer than on Earth, 2016 is an unusually long year on our home planet. Not only was a leap day included, but a leap second will be added at the very end of the year to keep celestial navigators’ clocks in sync with nature. The Dawn team already has accounted for the extra second in the intricate plans formulated for the spacecraft. And at that second, on Dec. 31 at 23:59:60, we will be able to look back on 366 days and one second, an especially full and gratifying year in this remarkable deep-space expedition. But we needn’t wait. Even now, as mission control is bathed in a lovely glow, the members of the team as well as space enthusiasts everywhere are aglow with the thrill of new knowledge, the excitement of a daring, noble adventure and the anticipation of more to come.
Dawn is 3,150 miles (5,070 kilometers) from Ceres. It is also 2.08 AU (194 million miles, or 312 million kilometers) from Earth, or 770 times as far as the moon and 2.11 times as far as the sun today. Radio signals, traveling at the universal limit of the speed of light, take 35 minutes to make the round trip.
Dr. Marc D. Rayman
4:00 p.m. PST November 28, 2016
Sigh. Sometimes life feels heavy.
Even as the holidays approach and we’re all supposed to be in a holiday spirit, supposed to be joyous. Sometimes we’re just not there.
But, as always, NASA gives me the opportunity to look at Earth from the highest perspective. From above, the world appears remote and untouched. There’s nothing but the timeless, immaculate and infinite beauty of our planet.
Together, you and I get to take this opportunity to share thankfulness for our Earth and everything pristine and beautiful about it.
Thank you for reading. I really mean it.
Slow down and relax. Earth is beautiful.
Earth, from the vantage point of space: Serene, breathtaking, magnificent. No matter how crazy busy your day is, no matter the level of stress, or chaos, or distraction, take a moment today—right now, in fact—to step back and feast on the great wonder of our home planet, Earth.