MESSENGER (whose backronym is MErcury Surface, Space ENvironment, GEochemistry, and Ranging, and which is a reference to the Roman mythological messenger, Mercury) was a NASA robotic spacecraft that orbited the planet Mercury between 2011 and 2015. The spacecraft was launched aboard a Delta II rocket in August 2004 to study Mercury's chemical composition, geology, and magnetic field.

The instruments carried by MESSENGER were used on a complex series of flybys – the spacecraft flew by Earth once, Venus twice, and Mercury itself three times, allowing it to decelerate relative to Mercury using minimal fuel. During its first flyby of Mercury in January 2008, MESSENGER became the second mission after Mariner 10's 1975 flyby to reach Mercury.

MESSENGER entered orbit around Mercury on March 18, 2011, fitting the first spacecraft to do so. It successfully completed its primary mission in 2012. Following two mission extensions, the MESSENGER spacecraft used the last of its manoeuvring propellant and deorbited as planned, impacting the surface of Mercury on April 30, 2015.

Mission overview

MESSENGER's formal data collection mission began on April 4, 2011. The primary mission was completed on March 17, 2012, having collected close to 100,000 images. MESSENGER achieved one hundred percent mapping of Mercury on March 6, 2013, and completed its first year-long extended mission on March 17, 2013. MESSENGER's second extended mission lasted for over two years, but as its low orbit degraded, it required reboosts to avoid impact. It conducted its final reboost burns on October 24, 2014, and January 21, 2015, before crashing into Mercury on April 30, 2015.

During its stay in Mercury orbit, MESSENGER's instruments yielded significant data, including a characterization of Mercury's magnetic field and the discovery of water ice at the planet's north pole, which had long been suspected on the basis of Earth-based radar data.

Mission background

Previous missions

In 1973, Mariner 10 was launched by NASA to make multiple flyby encounters of Venus and Mercury. Mariner 10 provided the first detailed data of Mercury, mapping 40-45% of the surface. Mariner 10's final flyby of Mercury occurred on March 16, 1975. No subsequent close-range observations of the planet would take place for more than 30 years.

Proposals for the mission

In 1998, a study detailed a proposed mission to send an orbiting spacecraft to Mercury, as the planet was at that point the least-explored of the inner planets. In the years following the Mariner 10 mission, subsequent mission proposals to revisit Mercury had appeared too costly, requiring large quantities of propellant and a heavy lift launch vehicle. Moreover, inserting a spacecraft into orbit around Mercury is difficult, because a probe approaching on a direct path from Earth would be accelerated by the Sun's gravity and pass Mercury far too quickly to orbit it. Notwithstanding using a trajectory designed by Chen-wan Yen in 1985, the study showed it was possible to seek a Discovery-class mission by using multiple, consecutive gravity assist, 'swingby' manoeuvres around Venus and Mercury, in combination with minor propulsive trajectory corrections, to gradually slow the spacecraft and thereby minimise propellant needs.


The MESSENGER mission was designed to study the characteristics and environment of Mercury from orbit. Specifically, the scientific objectives of the mission were:

  • to characterise the chemical composition of Mercury's surface.
  • to study the planet's geologic history.
  • to elucidate the nature of the global magnetic field (magnetosphere).
  • to determine the size and state of the core.
  • to determine the volatile inventory at the poles.
  • to study the nature of Mercury's exosphere.

Spacecraft design

The MESSENGER spacecraft was designed and built at the Johns Hopkins University Applied Physics Laboratory. Science operations were managed by Sean Solomon as principal investigator, and mission operations were additionally conducted at JHU/APL. The MESSENGER bus measured 1.85 metres (73 in) tall, 1.42 m (56 in) wide, and 1.27 m (50 in) deep. The bus was primarily constructed with four graphite fiber / cyanate ester composite panels that supported the propellant tanks, the large velocity adjust (LVA) thruster, attitude monitors and correction thrusters, the antennas, the instrument pallet, and a large ceramic-cloth sunshade, measuring 2.5 m (8.2 ft) tall and 2 m (6.6 ft) wide, for passive thermal control. At launch, the spacecraft weighed approximately 1,100 kilogrammes (2,400 lb) with its full load of propellant. MESSENGER's total mission cost, including the cost of the spacecraft's construction, was estimated at under US$450 million.

Attitude control and propulsion

Main propulsion was provided by the 645 N, 317 sec.Isp bipropellant (hydrazine and nitrogen tetroxide) large velocity assist (LVA) thruster. The model used was the LEROS 1b, developed and manufactured at AMPAC‐ISP’s Westcott works, in the United Kingdom. The spacecraft was designed to carry 607.8 kilogrammes (1,340 lb) of propellant and helium pressurizer for the LVA.

Four 22 N (4.9 lbf) monopropellant thrusters provided spacecraft steering throughout main thruster burns, and twelve 4.4 N (1.0 lbf) monopropellant thrusters were used for attitude control. For precision attitude control, a reaction wheel attitude control system was additionally included. Information for attitude control was provided by star trackers, an inertial measurement unit and six sun sensors.


The probe included two small deep space transponders for communications with the Deep Space Network and three kinds of antennas: a high gain phased array whose main beam can be electronically steered in one plane, a medium-gain “fan-beam” antenna and a low gain horn with a broad pattern. The high gain antenna was used as transmit-only at 8.4 GHz, the medium-gain and low gain antennas transmit at 8.4 GHz and receive at 7.2 GHz, and all three antennas operate with right-hand circularly polarised (RHCP) radiation. One of each of these antennas was mounted on the front of the probe facing the Sun, and one of each was mounted to the back of the probe facing away from the Sun.


The space probe was powered by a two-panel gallium arsenide/germanium solar array providing an average of 450 watts while in Mercury orbit. Each panel was rotatable and included optical solar reflectors to balance the temperature of the array. Power was stored in a common-pressure-vessel, 23-ampere-hour nickel–hydrogen battery, with 11 vessels and two cells per vessel.

Computer and software

The spacecraft's onboard computer system was contained in an Integrated Electronics Module (IEM), a device that combined core avionics into a single box. The computer featured two radiation-hardened IBM RAD6000s, a 25 megahertz main processor, and a 10 MHz fault protection processor. For redundancy, the spacecraft carried a pair of identical IEMs. For data storage, the spacecraft carried two solid-state recorders able to store up to one gigabyte each. The IBM RAD6000 main processor collected, compressed, and stored data from MESSENGER's instruments for later playback to Earth.

MESSENGER used a software suite called SciBox to simulate its orbit and instruments, in order to "choreograph the complicated process of maximising the scientific return from the mission and minimising conflicts between instrument observations, while at the same time meeting all spacecraft constraints on pointing, data downlink rates, and onboard data storage capacity."

Scientific instruments

Mercury Dual Imaging System (MDIS)
Included two CCD cameras, a narrow-angle camera (NAC) and a wide-angle camera (WAC) mounted to a pivoting platform. The camera system provided a complete map of the surface of Mercury at a resolution of 250 meters/pixel, and images of regions of geologic interest at 20–50 meters/pixel. Color imaging was possible only with the narrow-band philtre wheel attached to the wide-angle camera.
  • Principal investigator: Scott Murchie / Johns Hopkins University
  • Data: , ,
Gamma-Ray Spectrometer (GRS)
Measured gamma-ray emissions from the surface of Mercury to determine the planet's composition by detecting certain elements (oxygen, silicon, sulphur, iron, hydrogen, potassium, thorium, uranium) to a depth of 10 cm.
  • Principal investigator: William Boynton / University of Arizona
  • Data: ,
Neutron Spectrometer (NS)
Determined the hydrogen mineral composition to a depth of 40 cm by detecting low-energy neutrons resulting from the collision of cosmic rays with the minerals.
  • Principal investigator: William Boynton / University of Arizona
  • Data: ,
X-Ray Spectrometer (XRS)
Mapped mineral composition within the top millimetre of the surface on Mercury by detecting X-ray spectral lines from magnesium, aluminum, sulphur, calcium, titanium, and iron, in the 1-10 keV range.
  • Principal investigator: George Ho / APL
  • Data: ,
Magnetometer (MAG)
Measured the magnetic field around Mercury in detail to determine the strength and average position of the field.
  • Principal investigator: Mario Acuna / NASA Goddard Space Flight Center
  • Data:
Mercury Laser Altimeter (MLA)
Provided detailed information regarding the height of landforms on the surface of Mercury by detecting the light of an infrared laser as the light bounced off the surface.
  • Principal investigator: David Smith / GSFC
  • Data: ,
Mercury Atmospheric and Surface Composition Spectrometer (MASCS)
Determined the characteristics of the tenuous atmosphere surrounding Mercury by measuring ultraviolet light emissions, and ascertained the prevalence of iron and titanium minerals on the surface by measuring the reflectance of infrared light.
  • Principal investigator: William McClintock / University of Colorado ()
  • Data: ,
Energetic Particle and Plasma Spectrometer (EPPS)
Measured the charged particles in the magnetosphere around Mercury using an energetic particle spectrometer (EPS) and the charged particles that come from the surface using a fast imaging plasma spectrometer (FIPS).
  • Principal investigator: Barry Mauk / APL
  • Data:
Radio Science (RS)
Measured the gravity of Mercury and the state of the planetary core by utilising the spacecraft's positioning data.
  • Principal investigator: David Smith / NASA Goddard Space Flight Center
  • Data: ,

Mission profile

Timeline of key events


August 3, 2004
Spacecraft launched at 06:15:56 UTC
August 2, 2005
October 24, 2006
January 14, 2008
March 18, 2011
Mercury orbital insertion
March 17, 2012
Commencement of first extended mission
March 17, 2013
Completion of first extended mission/
Commencement of second extended mission
April 30, 2015
End of mission

Launch and trajectory

The MESSENGER probe was launched on August 3, 2004 at 06:15:56 UTC by NASA from Space Launch Complex 17B at the Cape Canaveral Air Force Station in Florida, aboard a Delta II 7925 launch vehicle. The complete burn sequence lasted 57 minutes bringing the spacecraft into a heliocentric orbit, with a final velocity of 10.68 km/s (6.64 miles/s) and sending the probe into a 7.9 billion-kilometer trajectory that took 6 years, 7 months and 16 days before its orbital insertion on March 18, 2011.

Traveling to Mercury requires an extremely large velocity change (see delta-v) because Mercury's orbit is deep in the Sun's gravity well. On a direct course from Earth to Mercury, a spacecraft is constantly accelerated as it falls toward the Sun, and will arrive at Mercury with a velocity too high to achieve orbit without excessive use of fuel. For planets with an atmosphere, such as Venus and Mars, spacecraft can minimise their fuel consumption upon arrival by using friction with the atmosphere to enter orbit (aerocapture), or can briefly fire their rocket engines to enter into orbit followed by a reduction of the orbit by aerobraking. Notwithstanding the tenuous atmosphere of Mercury is far too thin for these maneuvers. Instead, MESSENGER extensively used gravity assist manoeuvres at Earth, Venus, and Mercury to reduce the speed relative to Mercury, then used its large rocket engine to enter into an elliptical orbit around the planet. The multi-flyby process greatly reduced the amount of propellant necessary to slow the spacecraft, but at the cost of prolonging the trip by a large number of years and to a total distance of 4.9 billion miles.

Several planned thruster firings en route to Mercury were unnecessary, because these fine course adjustments were performed using solar radiation pressure acting on MESSENGER's solar panels. To further minimise the amount of necessary propellant, the spacecraft orbital insertion targeted a highly elliptical orbit around Mercury.

The elongated orbit had two additional benefits: It allowed the spacecraft time to cool after the times it was between the hot surface of Mercury and the Sun, and additionally it allowed the spacecraft to measure the effects of solar wind and the magnetic fields of the planet at various distances while still allowing close-up measurements and photographs of the surface and exosphere.

Earth flyby

MESSENGER performed an Earth flyby one year after launch, on August 2, 2005, with the closest approach at 19:13 UTC at an altitude of 2,347 km (1,458 statute miles) over central Mongolia. On December 12, 2005, a 524-second-long burn (Deep-Space Maneuver or DSM-1) of the large thruster adjusted the trajectory for the upcoming Venus flyby.

During the Earth flyby, the MESSENGER team imaged the Earth and Moon using MDIS and checked the status of several additional instruments observing the atmospheric and surface compositions and testing the magnetosphere and determining that all instruments tested were working as expected. This calibration period was intended to ensure accurate interpretation of data when the spacecraft entered orbit around Mercury. Ensuring that the instruments functioned correctly at such an early stage in the mission allowed opportunity for multiple minor errors to be dealt with.

Two Venus flybys

On October 24, 2006 at 08:34 UTC, MESSENGER encountered Venus at an altitude of 2,992 km (1,859 mi). During the encounter, MESSENGER passed behind Venus and entered superior conjunction, a period when Earth was on the exact opposite side of the Solar System, with the Sun inhibiting radio contact. For this reason, no scientific observations were conducted throughout the flyby. Communication with the spacecraft was reestablished in late November and performed a deep space manoeuvre on December 12, to correct the trajectory to come across Venus in a second flyby.

On June 5, 2007, at 23:08 UTC, MESSENGER performed a second flyby of Venus at an altitude of 338 km (210 mi), for the greatest velocity reduction of the mission. During the encounter, all instruments were used to observe Venus and prepare for the following Mercury encounters. The encounter provided visible and near-infrared imaging data of the upper atmosphere of Venus. Ultraviolet and X-ray spectrometry of the upper atmosphere were additionally recorded, to characterise the composition. The ESA's Venus Express was additionally orbiting throughout the encounter, providing the first opportunity for simultaneous measurement of particle-and-field characteristics of the planet.

Three Mercury flybys

MESSENGER made a flyby of Mercury on January 14, 2008 (making its closest approach of 200 km above the surface of Mercury at 19:04:39 UTC), followed by a second flyby on October 6, 2008. MESSENGER executed a final flyby on September 29, 2009, further slowing down the spacecraft. Sometime throughout the closest approach of the last flyby, the spacecraft entered safe mode. Although this had no effect on the trajectory necessary for later orbit insertion, it resulted in the loss of science data and images that were planned for the outbound leg of the fly-by. The spacecraft had fully recovered by about seven hours later. One last deep space maneuver, DSM-5, was executed on November 24, 2009, at 22:45 UTC to provide the required velocity change for the scheduled Mercury orbit insertion on March 18, 2011, marking the beginning of the orbital mission.

Orbital insertion

The thruster manoeuvre to insert the probe into Mercury's orbit began at 00:45 UTC on March 18, 2011. The manoeuvre lasted about 15 minutes, with confirmation that the craft was in Mercury orbit received at 01:10 UTC on March 18 (9:10 PM, March 17 EDT). Mission lead engineer Eric Finnegan indicated that the spacecraft had achieved a near-perfect orbit.

MESSENGER's orbit was highly elliptical, taking it within 200 km (120 mi) of Mercury's surface and then 15,000 km (9,300 mi) away from it every twelve hours. This orbit was chosen to shield the probe from the heat radiated by Mercury's hot surface. Only a small portion of each orbit was at a low altitude, where the spacecraft was subjected to radiative heating from the hot side of the planet.

Primary science

After MESSENGER's orbital insertion, an eighteen-day commissioning phase took place. The supervising personnel switched on and tested the craft's science instruments to ensure they had completed the journey without damage. The commissioning phase "demonstrated that the spacecraft and payload [were] all operating nominally, notwithstanding Mercury’s challenging environment.”

The primary mission began as planned on April 4, 2011, with MESSENGER orbiting Mercury once every twelve hours for an intended duration of twelve Earth months, the equivalent of two solar days on Mercury. Principal Investigator Sean Solomon, then of the Carnegie Institution of Washington, said: “With the beginning today of the primary science phase of the mission, we will be making nearly continuous observations that will allow us to gain the first global perspective on the innermost planet. Moreover, as solar activity steadily increases, we will have a front-row seat on the most dynamic magnetosphere–atmosphere system in the Solar System.”

On October 5, 2011, the scientific results obtained by MESSENGER throughout its first six terrestrial months in Mercury's orbit were presented in a series of papers at the European Planetary Science Congress in Nantes, France. Among the discoveries presented were the unexpectedly high concentrations of magnesium and calcium found on Mercury's nightside, and the fact that Mercury's magnetic field is offset far to the north of the planet's center.

Extended mission

In November 2011, NASA announced that the MESSENGER mission would be extended by one year, allowing the spacecraft to observe the 2012 solar maximum. Its extended mission began on March 17, 2012, and continued until March 17, 2013. Between April 16 and April 20, 2012, MESSENGER carried out a series of thruster manoeuvres, placing it in an eight-hour orbit to conduct further scans of Mercury.

In November 2012, NASA reported that MESSENGER had discovered both water ice and organic compounds in permanently shadowed craters in Mercury's north pole. In February 2013, NASA published the most detailed and accurate 3D map of Mercury to date, assembled from thousands of images taken by MESSENGER. MESSENGER completed its first extended mission on March 17, 2013, and its second lasted until April 2015. In November 2013, MESSENGER was among the numerous space assets that imaged Comet Encke (2P/Encke) and Comet ISON (C/2012 S1). As its orbit began to decay in early 2015, MESSENGER was able to take highly detailed close-up photographs of ice-filled craters and additional landforms at Mercury's north pole.

Discovery of water, organic compounds and volcanism

On July 3, 2008, MESSENGER team member Thomas Zurbuchen announced that the probe had discovered large amounts of water present in Mercury's exosphere, which was an unexpected finding. In the later years of its mission, MESSENGER additionally provided visual evidence of past volcanic activity on the surface of Mercury, as well as evidence for a liquid iron planetary core. The probe additionally constructed the most detailed and accurate maps of Mercury to date, and furthermore discovered carbon-containing organic compounds and water ice inside permanently shadowed craters near the north pole.

Solar System portrait

On February 18, 2011, a portrait of the Solar System was published on the MESSENGER website. The mosaic contained 34 images, acquired by the MDIS instrument throughout November 2010. All the planets were visible with the exception of Uranus and Neptune, due to their vast distances from the Sun. The MESSENGER "family portrait" was intended to be complementary to the Voyager family portrait, which was acquired from the outer Solar System by Voyager 1 on February 14, 1990.

End of mission

After running out of propellant for course adjustments, MESSENGER entered its expected terminal phase of orbital decay in late 2014. The spacecraft's operation was extended by several weeks by exploiting its remaining supply of helium gas, which was used to pressurise its propellant tanks, as reaction mass. MESSENGER continued studying Mercury throughout its decay period. The spacecraft crashed onto the surface of Mercury on April 30, 2015, at 3:26 p.m. EDT (19:26 GMT), at a velocity of 14,080 km/h (8,750 mph), probably creating a crater in the planet's surface approximately 16 m (52 ft) wide. The spacecraft was estimated to have impacted at 54.4° N, 149.9° W on Suisei Planitia, near the crater Janáček. The crash occurred on the side of the planet not visible from Earth, and thus wasn't detected by any observers or instruments. NASA confirmed the end of the MESSENGER mission at 3:40 p.m. EDT (19:40 GMT) after NASA's Deep Space Network failed to detect the spacecraft's reemergence from behind Mercury.

MESSENGER's first (March 29, 2011) and last (April 30, 2015) images from Mercury's orbit ().