Artist's illustration of Rosetta
|Mission type||Comet orbiter/lander|
|Mission duration||Final: 12 years, 6 months, 28 days|
|Launch mass||Orbiter: 2,900 kg (6,400 lb)
Lander: 100 kg (220 lb)
|Dry mass||Orbiter: 1,230 kg (2,710 lb)|
|Payload mass||Orbiter: 165 kg (364 lb)
Lander: 27 kg (60 lb)
|Dimensions||2.8 × 2.1 × 2 m (9.2 × 6.9 × 6.6 ft)|
|Power||850 watts at 3.4 AU|
|Start of mission|
|Launch date||2 March 2004, 07:17:51UTC|
|Rocket||Ariane 5G+ V-158|
|Launch site||Kourou ELA-3|
|End of mission|
|Last contact||30 September 2016, 10:39:28UTC SCET|
|Landing site||Sais, Ma'at region
2 years, 55 days of operations at the comet
|Flyby of Mars|
|Closest approach||25 February 2007|
|Distance||250 km (160 mi)|
|Flyby of 2867 Šteins|
|Closest approach||5 September 2008|
|Distance||800 km (500 mi)|
|Flyby of 21 Lutetia|
|Closest approach||10 July 2010|
|Distance||3,162 km (1,965 mi)|
|Orbital insertion||6 August 2014, 09:06 UTC|
|Periapsis||29 km (18 mi)|
|Band||S band (low gain antenna)
X band (high gain antenna)
|Bandwidth||from 7.8 bit/s (S band)
up to 91 kbit/s (X band)
Rosetta mission insignia
Rosetta was a space probe built by the European Space Agency launched on 2 March 2004. Along with Philae, its lander module, Rosetta performed a detailed study of comet 67P/Churyumov–Gerasimenko (67P). During its journey to the comet, the spacecraft flew by Mars and the asteroids 21 Lutetia and 2867 Šteins.
On 6 August 2014, the spacecraft reached the comet and performed a series of manoeuvres to be captured in its orbit. On 12 November, its lander module Philae performed the first successful landing on a comet, though its battery power ran out two days later. Communications with Philae were briefly restored in June and July 2015, but due to diminishing solar power, Rosetta's communications module with the lander was turned off on 27 July 2016. On 30 September 2016, the Rosetta spacecraft ended its mission by landing on the comet in its Ma'at region.
The probe is named after the Rosetta Stone, a stele of Egyptian origin featuring a decree in three scripts. The lander is named after the Philae obelisk, which bears a bilingual Greek and Egyptian hieroglyphic inscription.
- 1 Mission overview
- 2 History
- 3 Instruments
- 4 Search for organic compounds
- 5 Timeline of major events and discoveries
- 6 See also
- 7 References
- 8 External links
Rosetta was launched on 2 March 2004 from the Guiana Space Centre in French Guiana on an Ariane 5 rocket and reached Comet Churyumov–Gerasimenko on 6 August 2014, becoming the first spacecraft to orbit a comet. (Previous missions had conducted successful flybys of seven other comets.) It was one of ESA's Horizon 2000 cornerstone missions. The spacecraft consisted of the Rosetta orbiter, which featured 12 instruments, and the Philae lander, with nine additional instruments. The Rosetta mission orbited Comet Churyumov–Gerasimenko for 17 months and was designed to complete the most detailed study of a comet ever attempted. The spacecraft was controlled from the European Space Operations Centre (ESOC), in Darmstadt, Germany. The planning for the operation of the scientific payload, together with the data retrieval, calibration, archiving and distribution, was performed from the European Space Astronomy Centre (ESAC), in Villanueva de la Cañada, near Madrid, Spain. It has been estimated that in the decade preceding 2014, some 2,000 people assisted in the mission in some capacity.
In 2007, Rosetta made a Mars gravity assist (flyby) on its way to Comet Churyumov–Gerasimenko. The spacecraft also performed two asteroid flybys. The craft completed its flyby of asteroid 2867 Šteins in September 2008 and of 21 Lutetia in July 2010. Later, on 20 January 2014, Rosetta was taken out of a 31-month hibernation mode as it approached Comet Churyumov–Gerasimenko.
Rosetta's Philae lander successfully made the first soft landing on a comet nucleus when it touched down on Comet Churyumov–Gerasimenko on 12 November 2014. On 5 September 2016, ESA announced that the lander was discovered by the narrow-angle camera aboard Rosetta as the orbiter made a low, 2.7 km (1.7 mi) pass over the comet. The lander sits on its side wedged into a dark crevice of the comet, explaining the lack of electrical power to establish proper communication with the orbiter.
During the 1986 approach of Halley's Comet, international space probes were sent to explore the comet, most prominent among them being ESA's Giotto. After the probes returned valuable scientific information, it became obvious that follow-ons were needed that would shed more light on cometary composition and answer new questions.
Both ESA and NASA started cooperatively developing new probes. The NASA project was the Comet Rendezvous Asteroid Flyby (CRAF) mission. The ESA project was the follow-on Comet Nucleus Sample Return (CNSR) mission. Both missions were to share the Mariner Mark II spacecraft design, thus minimising costs. In 1992, after NASA cancelled CRAF due to budgetary limitations, ESA decided to develop a CRAF-style project on its own. By 1993 it was evident that the ambitious sample return mission was infeasible with the existing ESA budget, so the mission was redesigned and subsequently approved by the ESA, with the final flight plan resembling the cancelled CRAF mission: an asteroid flyby followed by a comet rendezvous with in-situ examination, including a lander. After the spacecraft launch, Gerhard Schwehm was named mission manager; he retired in March 2014.
The probe is named after the Rosetta Stone, a stele of Egyptian origin featuring a decree in three scripts. The lander is named after the Philae obelisk, which bears a bilingual Greek and Egyptian hieroglyphic inscription. A comparison of its hieroglyphs with those on the Rosetta Stone catalysed the deciphering of the Egyptian writing system. Similarly, it is hoped that these spacecraft will result in better understanding of comets and the early Solar System. In a more direct analogy to its namesake, the Rosetta spacecraft also carries a micro-etched nickel alloy Rosetta disc donated by the Long Now Foundation inscribed with 13,000 pages of text in 1,200 languages.
The Rosetta mission achieved many historic firsts.
On its way to comet 67P, Rosetta passed through the main asteroid belt, and made the first European close encounter with several of these primitive objects. Rosetta was the first spacecraft to fly close to Jupiter's orbit using solar cells as its main power source.
Rosetta was the first spacecraft to orbit a comet nucleus, and was the first spacecraft to fly alongside a comet as it headed towards the inner Solar System. It became the first spacecraft to examine at close proximity the activity of a frozen comet as it is warmed by the Sun. Shortly after its arrival at 67P, the Rosetta orbiter dispatched the Philae lander for the first controlled touchdown on a comet nucleus. The robotic lander's instruments obtained the first images from a comet's surface and made the first in situ analysis of its composition.
Design and construction
The Rosetta bus is a 2.8 × 2.1 × 2.0 m (9.2 × 6.9 × 6.6 ft) central frame and aluminium honeycomb platform. Its total mass is approximately 3,000 kg (6,600 lb), which includes the 100 kg (220 lb) Philae lander and 165 kg (364 lb) of science instruments. The Payload Support Module is mounted on top of the spacecraft and houses the scientific instruments, while the Bus Support Module is on the bottom and contains spacecraft support subsystems. Heaters placed around the spacecraft keep its systems warm while it is distant from the Sun. Rosetta's communications suite includes a 2.2 m (7.2 ft) steerable high-gain parabolic dish antenna, a 0.8 m (2.6 ft) fixed-position medium-gain antenna, and two omnidirectional low-gain antennas.
Electrical power for the spacecraft comes from two solar arrays totalling 64 square metres (690 sq ft). Each solar array is subdivided into five solar panels, with each panel being 2.25 × 2.736 m (7.38 × 8.98 ft). The individual solar cells are made of silicon, 200 μm thick, and 61.95 × 37.75 mm (2.44 × 1.49 in). The solar arrays generate a maximum of approximately 1,500 watts at perihelion, a minimum of 400 watts in hibernation mode at 5.2 AU, and 850 watts when comet operations begin at 3.4 AU. Spacecraft power is controlled by a redundant Terma power module also used in the Mars Express spacecraft, and is stored in four 10-A·h NiCd batteries supplying 28 volts to the bus.
Main propulsion comprises 24 paired bipropellant 10 N thrusters, with four pairs of thrusters being used for delta-v burns. The spacecraft carried 1,719.1 kg (3,790 lb) of propellant at launch: 659.6 kg (1,454 lb) of monomethylhydrazine fuel and 1,059.5 kg (2,336 lb) of dinitrogen tetroxide oxidiser, contained in two 1,108-litre (244 imp gal; 293 US gal) grade 5 titanium alloy tanks and providing delta-v of at least 2,300 metres per second (7,500 ft/s) over the course of the mission. Propellant pressurisation is provided by two 68-litre (15 imp gal; 18 US gal) high-pressure helium tanks.
Rosetta was built in a clean room according to COSPAR rules, but "sterilisation [was] generally not crucial since comets are usually regarded as objects where you can find prebiotic molecules, that is, molecules that are precursors of life, but not living microorganisms", according to Gerhard Schwehm, Rosetta's project scientist. The total cost of the mission is about €1.3 billion (US$1.8 billion).
Rosetta was set to be launched on 12 January 2003 to rendezvous with the comet 46P/Wirtanen in 2011. This plan was abandoned after the failure of an Ariane 5 carrier rocket during Hot Bird 7's launch on 11 December 2002, grounding it until the cause of the failure could be determined. In May 2003, a new plan was formed to target the comet 67P/Churyumov–Gerasimenko, with a revised launch date of 26 February 2004 and comet rendezvous in 2014. The larger mass and the resulting increased impact velocity made modification of the landing gear necessary.
After two scrubbed launch attempts, Rosetta was launched on 2 March 2004 at 07:17 UTC from the Guiana Space Centre in French Guiana. Aside from the changes made to launch time and target, the mission profile remained almost identical. Both co-discoverers of the comet, Klim Churyumov and Svetlana Gerasimenko, were present at the spaceport during the launch.
Deep space manoeuvres
To achieve the required velocity to rendezvous with 67P, Rosetta used gravity assist manoeuvres to accelerate throughout the inner Solar System. The comet's orbit was known before Rosetta's launch, from ground-based measurements, to an accuracy of approximately 100 km (62 mi). Information gathered by the onboard cameras beginning at a distance of 24 million kilometres (15,000,000 mi) were processed at ESA's Operation Centre to refine the position of the comet in its orbit to a few kilometres.
On 25 February 2007, the craft was scheduled for a low-altitude flyby of Mars, to correct the trajectory. This was not without risk, as the estimated altitude of the flyby was a mere 250 kilometres (160 mi). During that encounter, the solar panels could not be used since the craft was in the planet's shadow, where it would not receive any solar light for 15 minutes, causing a dangerous shortage of power. The craft was therefore put into standby mode, with no possibility to communicate, flying on batteries that were originally not designed for this task. This Mars manoeuvre was therefore nicknamed "The Billion Euro Gamble". The flyby was successful, with Rosetta even returning detailed images of the surface and atmosphere of the planet, and the mission continued as planned.
The second Earth flyby was on 13 November 2007 at a distance of 5,700 km (3,500 mi). In observations made on 7 and 8 November, Rosetta was briefly mistaken for a near-Earth asteroid about 20 m (66 ft) in diameter by an astronomer of the Catalina Sky Survey and was given the provisional designation 2007 VN84. Calculations showed that it would pass very close to Earth, which led to speculation that it could impact Earth. However, astronomer Denis Denisenko recognised that the trajectory matched that of Rosetta, which the Minor Planet Center confirmed in an editorial release on 9 November.
The spacecraft performed a close flyby of asteroid 2867 Šteins on 5 September 2008. Its onboard cameras were used to fine-tune the trajectory, achieving a minimum separation of less than 800 km (500 mi). Onboard instruments measured the asteroid from 4 August to 10 September. Maximum relative speed between the two objects during the flyby was 8.6 km/s (19,000 mph; 31,000 km/h).
Rosetta's third and final flyby of Earth happened on 12 November 2009.
On 10 July 2010, Rosetta flew by 21 Lutetia, a large main-belt asteroid, at a minimum distance of ±7.5 km ( 3,168±4.7 mi) at a velocity of 15 kilometres per second (9.3 mi/s). 1,969 The flyby provided images of up to 60 metres (200 ft) per pixel resolution and covered about 50% of the surface, mostly in the northern hemisphere. The 462 images were obtained in 21 narrow- and broad-band filters extending from 0.24 to 1 μm. Lutetia was also observed by the visible–near-infrared imaging spectrometer VIRTIS, and measurements of the magnetic field and plasma environment were taken as well.
In May 2014, Rosetta began a series of eight burns. These reduced the relative velocity between the spacecraft and 67P from 775 m/s (2,540 ft/s) to 7.9 m/s (26 ft/s).
Reaction control system problems
In 2006, Rosetta suffered a leak in its reaction control system (RCS). The system, which consists of 24 bipropellant 10-newton thrusters, was responsible for fine tuning the trajectory of Rosetta throughout its journey. The RCS operated at a lower pressure than designed due to the leak. While this may have caused the propellants to mix incompletely and burn 'dirtier' and less efficiently, ESA engineers were confident that the spacecraft would have sufficient fuel reserves to allow for the successful completion of the mission.
Rosetta's reaction wheels also showed higher than expected vibration, though testing revealed the system could be operated more efficiently resulting in less wear on the wheels. Before hibernation, two of the spacecraft's four reaction wheels began exhibiting "noise". Engineers turned on three of the wheels after the spacecraft awoke, including one of the bad wheels. The other improperly functioning wheel was held in reserve. Additionally, new software was uploaded which would allow Rosetta to function with only two active reaction wheels if necessary.
Orbit around 67P
In August 2014, Rosetta rendezvoused with the comet 67P/Churyumov–Gerasimenko (67P) and commenced a series of manoeuvres that took it on two successive triangular paths, averaging 100 and 50 kilometres (62 and 31 mi) from the nucleus, whose segments are hyperbolic escape trajectories alternating with thruster burns. After closing to within about 30 km (19 mi) from the comet on 10 September, the spacecraft entered actual orbit about it.[needs update]
The surface layout of 67P was unknown before Rosetta's arrival. The orbiter mapped the comet in anticipation of detaching its lander. By 25 August 2014, five potential landing sites had been determined. On 15 September 2014, ESA announced Site J, named Agilkia in honour of Agilkia Island by an ESA public contest and located on the "head" of the comet, as the lander's destination.
Philae detached from Rosetta on 12 November 2014 at 08:35 UTC, and approached 67P at a relative speed of about 1 m/s (3.6 km/h; 2.2 mph). It initially landed on 67P at 15:33 UTC, but bounced twice, coming to rest at 17:33 UTC. Confirmation of contact with 67P reached Earth at 16:03 UTC.
On contact with the surface, two harpoons were to be fired into the comet to prevent the lander from bouncing off as the comet's escape velocity is only around 1 m/s (3.6 km/h; 2.2 mph). Analysis of telemetry indicated that the surface at the initial touchdown site is relatively soft, covered with a layer of granular material about 0.82 feet (0.25 meters) deep, and that the harpoons had not fired upon landing. After landing on the comet, Philae had been scheduled to commence its science mission, which included:
- Characterisation of the nucleus
- Determination of the chemical compounds present, including amino acid enantiomers
- Study of comet activities and developments over time
Philae landed oddly, in the shadow of a nearby cliff and canted at an angle of around 30 degrees. This made it unable to adequately collect solar power, and it lost contact with Rosetta when its batteries ran out after two days, well before much of the planned science objectives could be attempted. Contact was briefly and intermittently reestablished several months later at various times between 13 June and 9 July, before contact was lost once again. There was no communication afterwards, and the transmitter to communicate with Philae was switched off in July 2016 to reduce power consumption of the probe. The precise location of the lander was discovered in September 2016 when Rosetta came closer to the comet and took high-resolution pictures of its surface. Knowing its exact location provides information needed to put Philae's two days of science into proper context.
Researchers expect the study of data gathered will continue for decades to come. One of the first discoveries was that the magnetic field of 67P oscillated at 40–50 millihertz. Scientists modified the signal by speeding it up 10,000 times so that people could hear a rendition of it. Although it is a natural phenomenon, it has been described as a "song" and has been compared to Continuum for harpsichord by György Ligeti. However, results from Philae's landing show that the comet's nucleus has no magnetic field, and that the field originally detected by Rosetta is likely caused by the solar wind.
The isotopic signature of water vapour from comet 67P, as determined by the Rosetta spacecraft, is substantially different from that found on Earth. That is, the ratio of deuterium to hydrogen in the water from the comet was determined to be three times that found for terrestrial water. This makes it very unlikely that water found on Earth came from comets such as comet 67P, according to the scientists. On 22 January 2015, NASA reported that, between June and August 2014, the rate at which water vapor was released by the comet increased up to tenfold.
On 2 June 2015, NASA reported that the ALICE spectrograph on Rosetta determined that electrons within 1 km (0.6 mi) above the comet nucleus — produced from photoionization of water molecules by solar radiation, and not photons from the Sun as thought earlier — are responsible for the degradation of water and carbon dioxide molecules released from the comet nucleus into its coma.
End of mission
As the orbit of comet 67P takes it farther from the Sun, the amount of sunlight reaching Rosetta's solar panels decreases. While it was possible to put Rosetta into a second hibernation phase during the comet's apohelion, there was no assurance that enough power would be available to run the spacecraft's heaters to keep it from freezing. In order to guarantee a maximum science return, mission managers made the decision to instead guide Rosetta down to the comet's surface and end the mission on impact, gathering photographs and instrument readings along the way. On 23 June 2015, at the same time as a mission extension was confirmed, ESA announced that end of mission would occur at the end of September 2016 after two years of operations at the comet.
Rosetta began a 19 km (12 mi) descent with a 208-second thruster burn executed on 29 September 2016 at approximately 20:50 UTC. Its trajectory targeted a site in the Ma'at region near an area of dust- and gas-producing active pits.
Impact on the comet's surface occurred 14.5 hours after its descent manoeuvre; the final data packet from Rosetta was transmitted at 10:39:28.895 UTC (SCET) by the OSIRIS instrument and was received at the European Space Operations Centre in Darmstadt, Germany, at 11:19:36.541 UTC. The spacecraft's estimated speed at the time of impact was 3.2 km/h (2.0 mph; 89 cm/s), and its touchdown location, named Sais by the operations team after the Rosetta Stone's original temple home, is believed to be only 40 m (130 ft) off-target. The final image transmitted by the spacecraft of the comet was taken by its OSIRIS instrument at an altitude of 20 m (66 ft) about 10 seconds before impact, showing an area 0.96 m (3.1 ft) across. Rosetta's computer included commands to send it into safe mode upon detecting that it had hit the comet's surface, turning off its radio transmitter and rendering it inert in accordance with International Telecommunication Union rules.
- ALICE (an ultraviolet imaging spectrograph). The ultraviolet spectrograph will search for and quantify the noble gas content in the comet nucleus, from which the temperature during the comet creation could be estimated. The detection is done by an array of potassium bromide and caesium iodide photocathodes. The 3.1 kg (6.8 lb) instrument uses 2.9 watts and was produced in the USA, and an improved version is used in the New Horizons spacecraft. It operates in the extreme and far ultraviolet spectrum, from 700–2,050 Å (70–205 nm).
- OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System). The camera system has a narrow-angle lens (700 mm) and a wide-angle lens (140 mm), with a 2048×2048 pixel CCD chip. The instrument was constructed in Germany.
- VIRTIS (Visible and Infrared Thermal Imaging Spectrometer). The Visible and IR spectrometer is able to make pictures of the nucleus in the IR and also search for IR spectra of molecules in the coma. The detection is done by a mercury cadmium telluride array for IR and with a CCD chip for the visible wavelength range. The instrument was produced in Italy, and improved versions were used for Dawn and Venus Express.
- MIRO (Microwave Instrument for the Rosetta Orbiter). The abundance and temperature of volatile substances like water, ammonia and carbon dioxide can be detected by MIRO via their microwave emissions. The 30 cm (12 in) radio antenna was constructed in Germany, while the rest of the 18.5 kg (41 lb) instrument was provided by the USA.
- CONSERT (Comet Nucleus Sounding Experiment by Radiowave Transmission). The CONSERT experiment will provide information about the deep interior of the comet using a radar. The radar will perform tomography of the nucleus by measuring electromagnetic wave propagation between the Philae lander and the Rosetta orbiter through the comet nucleus. This allows it to determine the comet's internal structure and deduce information on its composition. The electronics were developed by France and both antennas were constructed in Germany.
- RSI (Radio Science Investigation). RSI makes use of the probe's communication system for physical investigation of the nucleus and the inner coma of the comet.
Gas and particles
- ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis). The instrument consists of a double-focus magnetic mass spectrometer (DFMS) and a reflectron type time of flight mass spectrometer (RTOF). The DFMS has a high resolution (can resolve N2 from CO) for molecules up to 300 amu. The RTOF is highly sensitive for neutral molecules and for ions. ROSINA was developed at the University of Bern in Switzerland.
- MIDAS (Micro-Imaging Dust Analysis System). The high-resolution atomic force microscope will investigate several physical aspects of the dust particles which are deposited on a silicon plate.
- COSIMA (Cometary Secondary Ion Mass Analyser). COSIMA analyses the composition of dust particles by secondary ion mass spectrometry, using indium ions. It can detect ions up to a mass of 6500 amu.
- GIADA (Grain Impact Analyser and Dust Accumulator). GIADA will analyse the dust environment of the comet coma measuring the optical cross section, momentum, speed and mass of each grain entering inside the instrument.
Solar wind interaction
Search for organic compounds
Previous observations have shown that comets contain complex organic compounds. These are the elements that make up nucleic acids and amino acids, essential ingredients for life as we know it. Comets are thought to have delivered a vast quantity of water to Earth, and they may have also seeded Earth with organic molecules. Rosetta and Philae will also search for organic molecules, nucleic acids (the building blocks of DNA and RNA) and amino acids (the building blocks of proteins) by sampling and analysing the comet's nucleus and coma cloud of gas and dust, helping assess the contribution comets made to the beginnings of life on Earth. Before succumbing to falling power levels, Philae's COSAC instrument was able to detect organic molecules in the comet's atmosphere.
- Amino acids
Upon landing on the comet, Philae should have also tested some hypotheses as to why essential amino acids are almost all "left-handed", which refers to how the atoms arrange in orientation in relation to the carbon core of the molecule. Most asymmetrical molecules are oriented in approximately equal numbers of left- and right-handed configurations (chirality), and the primarily left-handed structure of essential amino acids used by living organisms is unique. One hypothesis that will be tested was proposed in 1983 by William A. Bonner and Edward Rubenstein, Stanford University professors emeritus of chemistry and medicine respectively. They conjectured that when spiralling radiation is generated from a supernova, the circular polarisation of that radiation could then destroy one type of "handed" molecules. The supernova could wipe out one type of molecules while also flinging the other surviving molecules into space, where they could eventually end up on a planet.
The mission has yielded a significant science return, collecting a wealth of data from the nucleus and its environment at various levels of cometary activity. The VIRTIS spectrometer on board the Rosetta spacecraft has provided evidence of nonvolatile organic macromolecular compounds everywhere on the surface of comet 67P with little to no water ice visible. Preliminary analyses strongly suggest the carbon is present as polyaromatic organic solids mixed with sulfides and iron-nickel alloys.
Solid organic compounds were also found in the dust particles emitted by the comet; the carbon in this organic material is bound in "very large macromolecular compounds", analogous to those found in carbonaceous chondrite meteorites. However, no hydrated minerals were detected, suggesting no link with carbonaceous chondrites.
In turn, the Philae lander's COSAC instrument detected organic molecules in the comet's atmosphere as it descended to its surface. Measurements by the COSAC and Ptolemy instruments on the Philae's lander revealed sixteen organic compounds, four of which were seen for the first time on a comet, including acetamide, acetone, methyl isocyanate and propionaldehyde. The only amino acid detected thus far on the comet is glycine, along with the precursor molecules methylamine and ethylamine.
Timeline of major events and discoveries
- 2 March – ESA's Rosetta mission was successfully launched at 07:17 UTC (04:17 local time) from Kourou, French Guiana.
- 4 March – Rosetta executed its first planned close swing-by (gravity assist passage) of Earth. The Moon and the Earth's magnetic field were used to test and calibrate the instruments on board of the spacecraft. The minimum altitude above the Earth's surface was 1,954.7 km (1,214.6 mi).
- 4 July – Imaging instruments on board observed the collision between the comet Tempel 1 and the impactor of the Deep Impact mission.
- 25 February – Mars flyby.
- 8 November – Catalina Sky Survey briefly misidentified the Rosetta spacecraft, approaching for its second Earth flyby, as a newly discovered asteroid.
- 13 November – Second Earth swing-by at a minimum altitude of 5,295 km (3,290 mi), travelling at 45,000 km/h (28,000 mph).
- 5 September – Flyby of asteroid 2867 Šteins. The spacecraft passed the main-belt asteroid at a distance of 800 km (500 mi) and the relatively slow speed of 8.6 km/s (31,000 km/h; 19,000 mph).
- 16 March – Observation of the dust tail of asteroid P/2010 A2. Together with observations by Hubble Space Telescope it could be confirmed that P/2010 A2 is not a comet, but an asteroid, and that the tail most likely consists of particles from an impact by a smaller asteroid.
- 10 July – Flew by and photographed the asteroid 21 Lutetia.
- May to July – Starting on 7 May, Rosetta began orbital correction manoeuvres to bring itself into orbit around 67P. At the time of the first deceleration burn Rosetta was approximately 2,000,000 km (1,200,000 mi) away from 67P and had a relative velocity of +775 m/s (2,540 ft/s); by the end of the last burn, which occurred on 23 July, the distance had been reduced to just over 4,000 km (2,500 mi) with a relative velocity of +7.9 m/s (18 mph). In total eight burns were used to align the trajectories of Rosetta 67P with the majority of the deceleration occurring during three burns: Delta-v's of 291 m/s (650 mph) on 21 May, 271 m/s (610 mph) on 4 June, and 91 m/s (200 mph) on 18 June.
- 14 July – The OSIRIS on-board imaging system returned images of comet 67P which confirmed the irregular shape of the comet.
- 6 August – Rosetta arrives at 67P, approaching to 100 km (62 mi) and carrying out a thruster burn that reduces its relative velocity to 1 m/s (3.3 ft/s). Commences comet mapping and characterisation to determine a stable orbit and viable landing location for Philae.
- 4 September – The first science data from Rosetta's ALICE instrument was reported, showing that the comet is unusually dark in ultraviolet wavelengths, hydrogen and oxygen are present in the coma, and no significant areas of water-ice have been found on the comet's surface. Water-ice was expected to be found as the comet is too far from the Sun to turn water into vapour.
- 10 September 2014 – Rosetta enters the Global Mapping Phase, orbiting 67P at an altitude of 29 km (18 mi).
- 12 November 2014 – Philae lands on the surface of 67P.
- 10 December 2014 – Data from the ROSINA mass spectrometers show that the ratio of heavy water to normal water on comet 67P is more than three times that on Earth. The ratio is regarded as a distinctive signature, and the discovery means that Earth's water is unlikely to have originated from comets like 67P.
- 14 April 2015 – Scientists report that the comet's nucleus has no magnetic field of its own.
- 2 July 2015 – Scientists report that active pits, related to sinkhole collapses and possibly associated with outbursts, have been found on the comet.
- 11 August 2015 – Scientists release images of a comet outburst that occurred on 29 July 2015.
- 28 October 2015 – Scientists publish an article in Nature reporting high levels of molecular oxygen around 67P.
- November 2014 to December 2015 – Rosetta escorted the comet around the Sun and performed riskier investigations.
- 27 July 2016 – ESA switched off the Electrical Support System Processor Unit (ESS) aboard Rosetta, disabling any possibility of further communications with the Philae lander.
- 2 September 2016 - Rosetta photographs the Philae lander for the first time after its landing, finding it wedged against a large overhang.
- 30 September 2016 - Mission ended in an attempt to slow land on the comet's surface near a 130 m (425 ft) wide pit called Deir el-Medina. The walls of the pit contain 0.91 m (3 ft) wide so-called "goose bumps", believed to represent the building blocks of the comet. Although Philae sent back some data during its descent, Rosetta has more powerful and more varied sensors and instruments, offering the opportunity to get some very close-in science to complement the more distant remote sensing it has been doing. The orbiter descended more slowly than Philae did.
The entire mission was featured heavily in social media, with a Facebook account for the mission and both the satellite and the lander having an official Twitter account portraying a personification of both spacecraft. The hashtag "#CometLanding" gained widespread traction. A Livestream of the control centres was set up, as were multiple official and unofficial events around the world to follow Philae's landing on 67P.
About Rosetta's mission
(9 min., 1080p HD, English)
About Philae's landing
(10 min., 1080p HD, English)
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|Wikimedia Commons has media related to Rosetta (spacecraft).|
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- Rosetta website at ESA.int
- Rosetta news site at ESA.int
- Rosetta operations site at ESA.int
- Rosetta website at NASA.gov
- Rosetta mission profile at NASA.gov