Artist's conception of Mars Global Surveyor
|Mission type||Mars orbiter|
|Operator||NASA / JPL|
|Mission duration||9 years, 11 months, 26 days from launch|
9 years, 1 month, 21 days (3249 sols) at Mars
En route: 10 months, 5 days
Aerobraking: 18 months, 20 days (552 sols)
Primary mission: 1 year, 9 months, 30 days (651 sols)
First: 1 year (355 sols)
Second: 11 months (326 sols)
First: 3 years, 9 months (1,332 sols)
Second: 33 days (32 sols)
|Launch mass||1,030.5 kg (2,272 lb)|
|Start of mission|
|Launch date||7 November 1996, 17:00UTC|
|Rocket||Delta II 7925|
|Launch site||Cape Canaveral LC-17A|
|End of mission|
|Last contact||2 November 2006|
|Semi-major axis||3,769 km (2,342 mi)|
|Periareion altitude||372.8 km (231.6 mi)|
|Apoareion altitude||436.5 km (271.2 mi)|
|Epoch||10 December 2004|
|Orbital insertion||11 September 1997, 01:17 UTC|
MSD 43972 16:29 AMT
Mars Global Surveyor (MGS) was an American robotic spacecraft developed by NASA's Jet Propulsion Laboratory and launched November 1996. Mars Global Surveyor was a global mapping mission that examined the entire planet, from the ionosphere down through the atmosphere to the surface. As part of the larger Mars Exploration Program, Mars Global Surveyor performed monitoring relay for sister orbiters during aerobraking, and it helped Mars rovers and lander missions by identifying potential landing sites and relaying surface telemetry.
It completed its primary mission in January 2001 and was in its third extended mission phase when, on 2 November 2006, the spacecraft failed to respond to messages and commands. A faint signal was detected three days later which indicated that it had gone into safe mode. Attempts to recontact the spacecraft and resolve the problem failed, and NASA officially ended the mission in January 2007.
Mars Global Surveyor achieved the following science objectives during its primary mission:
Mars Global Surveyor also achieved the following goals of its extended mission:
The Surveyor spacecraft, fabricated at the Lockheed Martin Astronautics plant in Denver, is a rectangular-shaped box with wing-like projections (solar panels) extending from opposite sides. When fully loaded with propellant at the time of launch, the spacecraft weighed 1,060 kg (2,337 lb). Most of Surveyor's mass lies in the box-shaped module occupying the center portion of the spacecraft. This center module is made of two smaller rectangular modules stacked on top of each other, one of which is called the equipment module and holds the spacecraft's electronics, science instruments, and the 1750A mission computer. The other module, called the propulsion module, houses Surveyor's rocket engines and propellant tanks. The Mars Global Surveyor mission cost about $154 million to develop and build and $65 million to launch. Mission operations and data analysis cost approximately $20 million/year.
The Mars Orbiter Camera (MOC) science investigation used 3 instruments: a narrow angle camera that took (black-and-white) high resolution images (usually 1.5 to 12 m per pixel) and red and blue wide angle pictures for context (240 m per pixel) and daily global imaging (7.5 km per pixel). MOC returned more than 240,000 images spanning portions of 4.8 Martian years, from September 1997 and November 2006. A high resolution image from MOC covers a distance of either 1.5 or 3.1 km long. Often, a picture will be smaller than this because it has been cut to just show a certain feature. These high resolution images may cover features 3 to 10 km long. When a high resolution image is taken, a context image is taken as well. The context image shows the image footprint of the high resolution picture. Context images are typically 115.2 km square with 240 m/pixel resolution.
The Mars Relay antenna supported the Mars Exploration Rovers for data relay back to Earth in conjunction with the Mars Orbiter Camera's 12 MB memory buffer. In total, more than 7.6 gigabits of data were transferred this way.
The Surveyor spacecraft was launched from the Cape Canaveral Air Station in Florida on 7 November 1996 aboard a Delta II rocket. The spacecraft traveled nearly 750 million kilometers (466 million miles) over the course of a 300-day cruise to reach Mars on 11 September 1997.
Upon reaching Mars, Surveyor fired its main rocket engine for the 22-minute Mars orbit insertion (MOI) burn. This maneuver slowed the spacecraft and allowed the planet's gravity to capture it into orbit. Initially, Surveyor entered a highly elliptical orbit that took 45 hours to complete. The orbit had a periapsis of 262 km (163 mi) above the northern hemisphere, and an apoapsis of 54,026 km (33,570 mi) above the southern hemisphere.
After orbital insertion, Surveyor performed a series of orbit changes to lower the periapsis of its orbit into the upper fringes of the Martian atmosphere at an altitude of about 110 km (68 mi). During every atmospheric pass, the spacecraft slowed down by a slight amount because of atmospheric resistance. The density of the Martian atmosphere at such altitudes is comparatively low, allowing this procedure to be performed without damage to the spacecraft. This slowing caused the spacecraft to lose altitude on its next pass through the orbit's apoapsis. Surveyor had planned to use this aerobraking technique over a period of four months to lower the high point of its orbit from 54,000 km (33,554 mi) to altitudes near 450 km (280 mi).
On 11 October, the flight team performed a maneuver to raise the periapsis out of the atmosphere. This suspension of aerobraking was performed because air pressure from the atmosphere caused one of Surveyor's two solar panels to bend backward by a slight amount. The panel in question was slightly damaged shortly after launch in November 1996. Aerobraking was resumed on 7 November after flight team members concluded that aerobraking was safe, provided that it occurs at a more gentle pace than proposed by the original mission plan.
Under the new mission plan, aerobraking occurred with the low point of the orbit at an average altitude of 120 km (75 mi), as opposed to the original altitude of 110 km (68 mi). This slightly higher altitude resulted in a decrease of 66 percent in terms of air resistance pressure experienced by the spacecraft. During these six months, aerobraking reduced the orbit period to between 12 and 6 hours.
From May to November 1998, aerobraking was temporarily suspended to allow the orbit to drift into the proper position with respect to the Sun. Without this hiatus, 'Surveyor' would complete aerobraking with its orbit in the wrong solar orientation. In order to maximize the efficiency of the mission, these six months were devoted to collecting as much science data as possible. Data was collected between two and four times per day, at the low point of each orbit.
Finally, from November 1998 to March 1999, aerobraking continued and shrank the high point of the orbit down to 450 km (280 mi). At this altitude, Surveyor circled Mars once every two hours. Aerobraking was scheduled to terminate at the same time the orbit drifted into its proper position with respect to the Sun. In the desired orientation for mapping operations, the spacecraft always crossed the day-side equator at 14:00 (local Mars time) moving from south to north. This geometry was selected to enhance the total quality of the science return.
The spacecraft circled Mars once every 117.65 minutes at an average altitude of 378 km (235 mi). It is in a near polar orbit (inclination = 93°) which is almost perfectly circular, moving from being over the south pole to being over the north pole in just under an hour. The altitude was chosen to make the orbit Sun-synchronous, so that all images that were taken by the spacecraft of the same surface features on different dates were taken under identical lighting conditions. After each orbit, the spacecraft viewed the planet 28.62° to the west because Mars had rotated underneath it. In effect, it was always 14:00 for Mars Global Surveyor as it moved from one time zone to the next exactly as fast as the Sun. After seven sols and 88 orbits, the spacecraft would approximately retrace its previous path, with an offset of 59 km to the east. This ensured eventual full coverage of the entire surface.
In its extended mission, MGS did much more than study the planet directly beneath it. It commonly performed rolls and pitches to acquire images off its nadir track. The roll maneuvers, called ROTOs (Roll Only Targeting Opportunities), rolled the spacecraft left or right from its ground track to shoot images as much as 30° from nadir. It was possible for a pitch maneuver to be added to compensate for the relative motion between the spacecraft and the planet. This was called a CPROTO (Compensation Pitch Roll Targeting Opportunity), and allowed for some very high resolution imaging by the onboard MOC (Mars Orbiting Camera).
In addition to this, MGS could shoot pictures of other orbiting bodies, such as other spacecraft and the moons of Mars. In 1998 it imaged what was later called the Phobos monolith, found in MOC Image 55103.
After analyzing hundreds of high-resolution pictures of the Martian surface taken by the orbiting Mars Surveyor spacecraft, a team of researchers found that weathering and winds on the planet create landforms, especially sand dunes, remarkably similar to those in some deserts on Earth.
Layers in Monument Valley. These are accepted as being formed, at least in part, by water deposition. Since Mars contains similar layers, water remains as a major cause of layering on Mars.
Buttes and layers in Aeolis quadrangle, as seen by Mars Global Surveyor.
Lava flows were once covered over, now these platy flows are being exposed.
Crater was buried, now it is being exhumed by erosion. Image located in Ismenius Lacus quadrangle.
The northern hemisphere appears smooth, but the craters are covered over. Here, a group of craters are partially exposed. Image located in Cebrenia quadrangle.
Gullies on one wall of Kaiser Crater. Gullies usually are found in only one wall of a crater.
Close up image of Phaethontis surface taken by Mars Global Surveyor, under MOC Public Targeting Program. Pits are thought to be caused by buried ice turning into a gas.
The mantle drapes most of the area. Note the absence of boulders on the cliff face. An area that shows the edges of the mantle is circled. Image located in Ismenius Lacus quadrangle.
Mantle material, as seen by MGS.
Dust devil, as seen by MGS.
Dust devil in action showing shadow to the right. Image located in Cebrenia quadrangle.
Changes in south pole from 1999 to 2001, as seen by Mars Global Surveyor. Notice how Swiss-cheese type holes have grown in the two years.
Swiss cheese terrain, as seen by MGS. Largest mesa in image is 4 meters high.
Layers in Swiss cheese terrain. There is a bright upper layer and a darker lower layer.
Close-up view of Swiss cheese terrain. Polygonal pattern was probably formed by shallow troughs.
Ceraunius Tholus, one of many volcanoes found on Mars.
Lava flows in the Tharsis quadrangle.
Image shows both young and old lava flows from the base of Olympus Mons. The flat plain is the younger flow. The older flow has channels with levees along their edges. The presence of levees is quite common in many lava flows.
Small volcano in Phoenicis Lacus quadrangle. Image covers a distance 1.9 mi (3.1 km) long.
House-sized boulders are scattered throughout this image.
These boulders are near Ascraeus Mons, a Martian volcano. Volcanoes on Mars probably form hard boulders made up of basalt that is resistant to erosion in the current environment of Mars.
Many streaks underwent changes during the many years that MGS functioned.
Data from MGS have been used to perform a test of the general relativistic Lense–Thirring precession which consists of a small precession of the orbital plane of a test particle moving around a central, rotating mass such as a planet. The interpretation of these results has been debated.
On 6 December 2006 NASA released photos of two craters in Terra Sirenum and Centauri Montes which appear to show the presence of flowing water on Mars at some point between 1999 and 2001. The pictures were produced by Mars Global Surveyor and are quite possibly the spacecraft's final contribution to our knowledge of Mars and the question of whether water exists on the planet.
Hundreds of gullies were discovered that were formed from liquid water, possible in recent times. These gullies occur on steep slopes and mostly in certain bands of latitude.
On 2 November 2006, NASA lost contact with the spacecraft after commanding it to adjust its solar panels. Several days passed before a faint signal was received indicating that the spacecraft had entered safe mode and was awaiting further instructions.
On 21 and 22 November 2006, Mars Global Surveyor failed to relay communications to the Opportunity rover on the surface of Mars. In response to this complication, Mars Exploration Program manager Fuk Li stated, "Realistically, we have run through the most likely possibilities for re-establishing communication, and we are facing the likelihood that the amazing flow of scientific observations from Mars Global Surveyor is over."
On 13 April 2007, NASA announced the loss of the spacecraft was caused by a flaw in a parameter update to the spacecraft's system software. The spacecraft was designed to hold two identical copies of the system software for redundancy and error checking. Subsequent updates to the software encountered a human error when two independent operators updated separate copies with differing parameters. This was followed by a corrective update that unknowingly included a memory fault which resulted in the loss of the spacecraft.
Originally, the spacecraft was intended to observe Mars for 1 Martian year (approximately 2 Earth years). However, based on the vast amount of valuable science data returned, NASA extended the mission three times. The MGS remains in a stable near-polar circular orbit at about 450 km altitude, and will crash onto the surface of the planet in about 2047.
Image of possible CO
2 geysers, taken by Mars Global Surveyor and released on 16 October 2000.
Surface of Mars taken by Mars Global Surveyor.
Surface of Mars taken by Mars Global Surveyor.
Surface of Mars taken by Mars Global Surveyor on 10 August 1999.
Surface of Mars taken by Mars Global Surveyor on 10 August 1999.
The Mars rover Spirit's landing site and tracks taken by Mars Global Surveyor.
The Mars Express spacecraft image taken by Mars Global Surveyor.
The Mars Odyssey spacecraft image taken by Mars Global Surveyor.
Banded or taffy-pull terrain in Hellas, as seen by Mars Global Surveyor. Origin is unknown at present.
Bright rays caused by impact throwing out a bright lower layer. Some bright layers contain hydrated minerals. Picture taken by Mars Global Surveyor. Location is Memnonia quadrangle.
Mars Global Surveyor photograph of Opportunity rover's landing site showing "hole in one."
Inverted channels in Aeolis quadrangle. It is believed that stream channels became raised features after coarse materials were deposited and cemented.
Picture probably is of a delta that formed in a huge lake. The area is of great interest to geologists. Evidence of past microbial life may be found in this location.
Pavonis Mons, located on the equator in Tharsis quadrangle.
It's expected to orbit Mars for at least 50 years before crashing onto the surface of the planet.
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