67P/Churyumov–Gerasimenko

Template:Short description Template:Use American English Template:Use dmy dates {{#invoke:infobox|infoboxTemplate | class = vcard | titleclass = fn org | title = 67P/Churyumov–Gerasimenko | image = {{#invoke:InfoboxImage|InfoboxImage|image=File:Comet 67P True color.jpg|upright={{#if:||1.1}}|alt=}} | caption = Comet 67P/Churyumov–Gerasimenko in true colour, as seen by ESA's Rosetta spacecraft in December 2014 | headerstyle = {{#if:|background-color:|background-color:#E0CCFF}}; color:inherit; | labelstyle = max-width:{{#if:||11em}}; | autoheaders = y

| header1 = Discovery

| header10 = {{#if:|Designations|Designations}}

| header20 = Orbital characteristics{{#ifeq:|yes| (barycentric)}}<ref name="MPC"/>

| data21 = | data22 = {{#if:25 February 2023 (JD 2460000.5) |Epoch 25 February 2023 (JD 2460000.5)}} | data23 = {{#if: | Uncertainty parameter {{{uncertainty}}}}} | label24 = Observation arc | data24 = | label25 = Earliest precovery date | data25 = | label26 = {{#switch:{{{apsis}}} |apsis|gee|barion|center|centre|(apsis)=Apo{{{apsis}}} |Ap{{#if:|{{{apsis}}}|helion}}}} | data26 = Template:Convert | label27 = Peri{{#if:|{{{apsis}}}|helion}} | data27 = Template:Convert | label28 = Peri{{#if:|{{{apsis}}}|apsis}} | data28 = | label29 = {{#switch:{{{apsis}}} |helion|astron=Ap{{{apsis}}} |Apo{{#if:|{{{apsis}}}|apsis}}}} | data29 = | label30 = Periastron | data30 = | label31 = Apoastron | data31 = | label32 = Template:Longitem | data32 = Template:Convert | label33 = Template:Longitem | data33 = | label34 = Eccentricity | data34 = 0.64989 | label35 = Template:Longitem | data35 = 6.43 yr | label36 = Template:Longitem | data36 = | label37 = Template:Longitem | data37 = | label38 = Template:Longitem | data38 = 73.57° | label39 = Template:Longitem | data39 = | label40 = Inclination | data40 = 3.8719° | label41 = Template:Longitem | data41 = | label42 = Template:Longitem | data42 = 36.33° | label43 = Template:Longitem | data43 = | label44 = Template:Longitem | data44 = 9 April 2028<ref name="Horizons2028"/>
2 November 2021 (previous)<ref name="Yoshida"/><ref name=MPC/> | label45 = Template:Longitem | data45 = 22.15° | label46 = Template:Nowrap | data46 = | label47 = Satellite of | data47 = | label48 = Group | data48 = | label49 = {{#switch: |yes|true=Satellites |Known satellites}} | data49 = | label50 = Star | data50 = | label51 = Earth MOID | data51 = | label52 = Mercury MOID | data52 = | label53 = Venus MOID | data53 = | label54 = Mars MOID | data54 = | label55 = Jupiter MOID | data55 = | label56 = Saturn MOID | data56 = | label57 = Uranus MOID | data57 = | label58 = Neptune MOID | data58 = | label59 = T_Jupiter | data59 =

| header60 = Proper orbital elements

| label61 = Template:Longitem | data61 = {{#if: |{{{p_semimajor}}} AU}} | label62 = Template:Longitem | data62 = | label63 = Template:Longitem | data63 = | label64 = Template:Longitem | data64 = {{#if: |{{{p_mean_motion}}} deg Template:\yr}} | label65 = Template:Longitem | data65 = {{#if:|{{#expr:360/1 round 5}} yr
({{#expr:365.25*360/1 round 3}} d) }} | label66 = Template:Longitem | data66 = {{#if:|{{{perihelion_rate}}} arcsec Template:\yr }} | label67 = Template:Longitem | data67 = {{#if:|{{{node_rate}}} arcsec Template:\yr}}

| header70 = Template:Anchor{{#if:| Physical characteristics|Physical characteristics}}

| label71 = Dimensions | data71 = Template:Plainlist | label72 = Template:Longitem | data72 = | label73 = Template:Longitem | data73 = | label74 = Template:Longitem | data74 = | label75 = Template:Longitem | data75 = | label76 = Flattening | data76 = | label77 = Circumference | data77 = | label78 = Template:Longitem | data78 = | label79 = Volume | data79 = Template:Cvt<ref name="mass density 2016"/> | label80 = Mass | data80 = Template:Val<ref name="mass density 2016"/> | label81 = Template:Longitem | data81 = Template:Cvt | label82 = Template:Longitem | data82 = | label83 = Template:Longitem | data83 = | label84 = Template:Longitem | data84 = est. 1 m/s<ref name="mpg20140121"/> | label85 = Template:Longitem | data85 = Template:Val<ref name="Mottola2014"/> | label86 = Template:Longitem | data86 = | label87 = Template:Longitem | data87 = | label88 = Template:Longitem | data88 = 52°<ref name="esa20150122"/> | label89 = Template:Longitem | data89 = 69.3°<ref name="esa20150122"/> | label90 = Template:Longitem | data90 = 64.1°<ref name="esa20150122"/> | label91 = Template:Longitem | data91 = | label92 = Template:Longitem | data92 = | label93 = {{#if: |Template:Longitem |Albedo}} | data93 = 0.06<ref name="esa20150122"/> | label94 = Temperature | data94 =

| data100 = {{#if:KelvinCelsiusFahrenheit|

Surface temp.	min	max
Kelvin	Template:0180	Template:0230
Celsius	Template:0−93	Template:0−43
Fahrenheit	−135	Template:0−45
{{{temp_name4}}}

}}

| header110 = Atmosphere

| below = {{#if:||Template:Reflist }}

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67P/Churyumov–Gerasimenko (abbreviated as 67P or 67P/C–G) is a Jupiter-family comet.<ref name="yfernandez"/> It is originally from the Kuiper belt<ref name="AP-20141210-SB"/> and has an orbital period of 6.45 years as of 2012,<ref name=jpldata/> a rotation period of approximately 12.4 hours,<ref name="Mottola2014"/> and a maximum velocity of Template:Cvt.<ref name="ESA-faq"/> Churyumov–Gerasimenko is approximately Template:Cvt at its longest and widest dimensions.<ref name="67P_size"/> It was first observed on photographic plates in 1969 by Soviet astronomers Klim Ivanovych Churyumov and Svetlana Ivanovna Gerasimenko, after whom it is named.Template:Efn It most recently came to perihelion (closest approach to the Sun) on 2 November 2021,<ref name=MPC/><ref name="Yoshida"/><ref name=Kinoshita/> and will next come to perihelion on 9 April 2028.<ref name="Horizons2028"/>

Churyumov–Gerasimenko was the destination of the European Space Agency's Rosetta mission, launched on 2 March 2004.<ref name=Krolikowska2003/><ref name="NASA-201401017"/><ref name="NYT-20140805"/> Rosetta rendezvoused with Churyumov–Gerasimenko on 6 August 2014<ref name="Fischer2014-08-06"/><ref name="Bauer2014"/> and entered orbit on 10 September 2014.<ref name="esa20140910"/> RosettaTemplate:'s lander, Philae, landed on the comet's surface on 12 November 2014, becoming the first spacecraft to land on a comet nucleus.<ref name="NASA-20141112-DCA"/><ref name="NYT-20141112-KC"/><ref name=bbcland/> On 30 September 2016, the Rosetta spacecraft ended its mission by landing on the comet in its Ma'at region.<ref name="newsci20160930"/><ref name="space20160930"/>

Discovery

Churyumov–Gerasimenko was discovered in 1969 by Klim Ivanovich Churyumov of Kyiv University's Astronomical Observatory,<ref name="iau61"/> who examined a photograph that had been exposed for comet Comas Solà by Svetlana Ivanovna Gerasimenko on 11 September 1969 at the Alma-Ata Astrophysical Institute, near Alma-Ata, the then-capital city of Kazakh Soviet Socialist Republic, Soviet Union. Churyumov found a cometary object near the edge of the plate, but assumed that this was comet Comas Solà.<ref name="Kronk"/>

After returning to his home institute in Kyiv, Churyumov examined all the photographic plates more closely. On 22 October, about a month after the photograph was taken, he discovered that the object could not be Comas Solà, because it was about 1.8 degrees off the expected position. Further scrutiny produced a faint image of Comas Solà at its expected position on the plate, thus proving the other object to be a different body.<ref name="Kronk"/>

Shape

File:Comet 67P-Churyumov-Gerasimenko.stl The comet consists of two lobes connected by a narrower neck, with the larger lobe measuring about Template:Cvt and the smaller one about Template:Cvt.<ref name="esa20150122"/> With each orbit the comet loses matter, as gas and dust are evaporated away by the Sun. It is estimated that a layer with an average thickness of about Template:Cvt is lost per orbit as of 2015.<ref name="Bertaux2015"/> The comet has a mass of approximately 10 billion tonnes.<ref name="mass density 2016"/>

The two-lobe shape of the comet is the result of a gentle, low-velocity collision of two objects, and is called a contact binary. The "terraces", layers of the interior of the comet that have been exposed by partial stripping of outer layers during its existence, are oriented in different directions in the two lobes, indicating that two objects fused to form Churyumov–Gerasimenko.<ref name="natgeo20150928"/><ref name="Massironi2015"/>

Surface

There are 26 distinct regions on Churyumov–Gerasimenko, with each named after an Egyptian deity; regions on the large lobe are named after gods, whereas those on the small lobe are named after goddesses. Nineteen regions were defined in the northern hemisphere prior to equinox.<ref name="ElMaarry2015"/><ref name="space20150719"/> Later, when the southern hemisphere became illuminated, seven more regions were identified using the same naming convention.<ref name="ElMaarry2016"/><ref name="esa20160224"/>

Region	Terrain	Region	Terrain	Region	Terrain
Ma'at	Dust covered	Ash	Dust covered	Babi	Dust covered
Seth	Pitted and brittle material	Hatmehit	Large-scale depression	Nut	Large-scale depression
Aten	Large-scale depression	Hapi	Smooth	Imhotep	Smooth
Anubis	Smooth	Maftet	Rock-like	Bastet	Rock-like
Serqet	Rock-like	Hathor	Rock-like	Anuket	Rock-like
Khepry	Rock-like	Aker	Rock-like	Atum	Rock-like
Apis	Rock-like	Khonsu	Rock-like	Bes	Rock-like
Anhur	Rock-like, rather friable	Geb	Rock-like	Sobek	Rock-like
Neith	Rock-like	Wosret	Rock-like

Gates

Features described as gates, twin prominences on the surface so named for their appearance,Template:Clarify were named after deceased members of the Rosetta team.<ref name="esablog20150928"/>

Name	Named after
C. Alexander Gate	Claudia Alexander
A. Coradini Gate	Angioletta Coradini

Surface changes

During RosettaTemplate:'s lifetime, many changes were observed on the comet's surface, particularly when the comet was close to perihelion.<ref name="ElMaarry2017"/><ref name="esa20170321"/><ref name="nasa20170321"/> These changes included evolving patterns of circular shapes in smooth terrains that at some point grew in size by a few meters per day.<ref name="Groussin2015"/><ref name="esa20150918"/> A fracture in the neck region was also observed to grow in size; boulders tens of meters wide were displaced, sometimes travelling more than 100 meters; and patches of the ground were removed to expose new features. A number of collapsing cliffs have also been observed. One notable example in December 2015 was captured by RosettaTemplate:'s NAVCAM as a bright patch of light shining from the comet. Rosetta scientists determined that a large cliff had collapsed, making it the first landslide on a comet known to be associated with an outburst of activity.<ref name="Pajola2017"/><ref name="wapo20170321"/> An apparent outburst of the comet was observed on 14 November 2021.<ref name="AST-20211119">Template:Cite news</ref> According to the researchers, "At the time of the outburst discovery with ZTF, the comet was 1.23 au from the Sun and 0.42 au from the Earth. The comet's last perihelion passage was on 2021 Nov 2.".<ref name="AST-20211119"/>

Cheops boulder

Cheops is the largest boulder on the surface of the comet, measuring up to 45 meters. It is located in the comet's larger lobe. It was named for the pyramid in Giza because its shape is similar to that of a pyramid.<ref>Template:Cite news</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Orbit and rotation

Epoch	Perihelion (AU)
Perihelion distance at different epochs<ref name="Kinoshita"/>
1821	2.44
1882	2.94
1956	2.74
1963	1.28
2021	1.21
2101	1.35
2223	≈ 0.8<ref name="Horizons2223"/>

Like the other comets of the Jupiter family, Churyumov–Gerasimenko probably originated in the Kuiper belt and was ejected towards the interior of the Solar System, where later encounters with Jupiter successively changed its orbit. These interactions will continue until the comet is eventually thrown out of the Solar System or collides with the Sun or a planet.

On 4 February 1959, a close encounter with Jupiter of Template:Convert<ref name="jpldata"/> moved Churyumov–Gerasimenko's perihelion inward from Template:Convert to Template:Convert, where it basically remains today.<ref name="Kinoshita"/> In November 2220 the comet will pass about Template:Convert from Jupiter<ref name="Dunn"/> which will move perihelion inwards to about Template:Convert from the Sun.<ref name="Horizons2223"/>

Before Churyumov–Gerasimenko's perihelion passage in 2009, its rotational period was 12.76 hours. During this perihelion passage, it decreased to 12.4 hours, which likely happened because of sublimation-induced torque.<ref name="Mottola2014"/>

2015 perihelion

Template:As of, Churyumov–Gerasimenko's nucleus had an apparent magnitude of roughly 20.<ref name="MPC"/> It came to perihelion on 13 August 2015.<ref name="Yoshida"/><ref name="AP-20150813"/> From December 2014 until September 2015, it had an elongation less than 45 degrees from the Sun.<ref name="MPC-emp"/> On 10 February 2015, it went through solar conjunction when it was 5 degrees from the Sun and was Template:Convert from Earth.<ref name="MPC-emp"/> It crossed the celestial equator on 5 May 2015 and became easiest to see from the Northern Hemisphere.<ref name="MPC-emp"/> Even right after perihelion when it was in the constellation of Gemini, it only brightened to about apparent magnitude 12, and required a telescope to be seen.<ref name="Yoshida"/> Template:As of, the comet had a total magnitude of about 20.<ref name="MPC"/>

2021 perihelion

The 2021 apparition marked the closest approach to Earth since 1982.<ref name="jpldata"/> The comet reached perihelion on 2 November 2021<ref name="Yoshida"/> and the closest approach to Earth was on November 12, 2021, at 00:50 UTC, at a distance of 38 million miles (61 million km).<ref name="earthsky2021"/> The comet brightened to an apparent magnitude of 9, meaning it was visible with amateur telescopes.<ref name="earthsky2021">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Two outbursts were observed during the apparition, on 2021 October 29.940 and November 17.864 UTC, −3.12 days and +15.81 days, respectively, from the perihelion date. During the first outburst the comet brightened by 0.26 ± 0.03 mag in the outburst, with a 27% increase in the effective geometric cross-section and total outburst dust mass of Template:Val. The second outburst caused a brightening of 0.49 ± 0.08 mag with effective geometric cross-section and total outburst dust mass 2.5 times larger than the first event.<ref>Template:Cite journal Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.</ref>

Exploration

Rosetta mission

{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}} Template:See also The Rosetta mission was the first mission to include an orbiter that accompanied a comet for several years, as well as a lander that collected close-up data from the comet's surface. The mission launched in 2004, arrived at comet 67P in 2014, and concluded with a touchdown on the comet's surface in 2016.

Advance work

Template:Multiple image As preparation for the Rosetta mission, Hubble Space Telescope pictures taken on 12 March 2003 were closely analysed. An overall 3D model was constructed and computer-generated images were created.<ref name="STScI-2003-26"/>

On 25 April 2012, the most detailed observations until that time were taken with the 2-meter Faulkes Telescope by N. Howes, G. Sostero and E. Guido while it was at its aphelion.Template:Citation needed

On 6 June 2014, water vapor was detected being released at a rate of roughly Template:Convert when Rosetta was Template:Cvt from Churyumov–Gerasimenko and Template:Convert from the Sun.<ref name="blog140623"/><ref name="NASA-20140630"/> On 14 July 2014, images taken by Rosetta showed that its nucleus is irregular in shape with two distinct lobes.<ref name="astronomy20140717"/> The size of the nucleus was estimated to be Template:Cvt.<ref name="skytel20140717"/> Two explanations for its shape were proposed at the time: that it was a contact binary, or that its shape may have resulted from asymmetric erosion due to ice sublimating from its surface to leave behind its lobed shape.<ref name="NYT-20140805"/><ref name="Bauer2014"/> By September 2015, mission scientists had determined that the contact binary hypothesis was unambiguously correct.<ref name="Massironi2015"/><ref name="esa20150928"/>

Rendezvous and orbit

Template:Multiple image Beginning in May 2014, RosettaTemplate:'s velocity was reduced by Template:Cvt with a series of thruster firings.<ref name="NYT-20140805"/><ref name="csm20140804"/> Ground controllers rendezvoused Rosetta with Churyumov–Gerasimenko on 6 August 2014.<ref name="Fischer2014-08-06"/><ref name="Bauer2014"/> This was done by reducing RosettaTemplate:'s relative velocity to Template:Cvt. Rosetta entered orbit on 10 September, at about Template:Cvt from the nucleus.<ref name="Fischer2014-08-06"/><ref name="Bauer2014"/><ref name="Lakdawalla2014-08-15"/>

Landing

Template:Further Descent of a small lander occurred on 12 November 2014. Philae is a Template:Cvt robotic probe that set down on the surface with landing gear.<ref name="NYT-20140805"/><ref name="NYT-20141110-KC"/> The landing site has been christened Agilkia in honor of Agilkia Island, where the temples of Philae Island were relocated after the construction of the Aswan Dam flooded the island.<ref name="bbcnews20141104"/> The acceleration due to gravity on the surface of Churyumov–Gerasimenko has been estimated for simulation purposes at 10⁻³ m/s²,<ref name="Hilchenbach2004"/> or about 1/10,000 of that on Earth.

Because of its low relative mass, landing on the comet relied on tools to anchor Philae to the surface. The probe had an array of mechanisms designed to manage Churyumov–Gerasimenko's low gravity, including a cold gas thruster, harpoons, landing-leg-mounted ice screws, and a flywheel to keep it oriented during its descent.<ref name="cnn20141113"/><ref name="register20141112"/><ref name="discovery20141112"/> During the event, the thruster and the harpoons failed to operate, and the ice screws did not gain a grip. The lander bounced twice and only came to rest when it made contact with the surface for the third time,<ref name="NASA-20141113-DCA"/> two hours after first contact.<ref name="skytel20141112"/>

Contact with Philae was lost on 15 November 2014 because of dropping battery power. The European Space Operations Centre briefly reestablished communications on 14 June 2015 and reported a healthy spacecraft but communications were lost again soon after.<ref name="nature20150614"/> On 2 September 2016, Philae was located in photographs taken by the Rosetta orbiter. It had come to rest in a crack with only its body and two legs visible. While the discovery solves the question of the lander's disposition, it also allows project scientists to properly contextualise the data it returned from the comet's surface.<ref name="skytel20160905"/>

Physical properties

The composition of water vapor from Churyumov–Gerasimenko, as determined by the Rosetta spacecraft, is substantially different from that found on Earth. 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 unlikely that water found on Earth came from comets like Churyumov–Gerasimenko.<ref name="AP-20141210-SB"/><ref name="NASA-20141210-DCA"/><ref name="NYT-20141210-KC"/> The water vapor is also mixed with significant amount of formaldehyde (0.5 wt%) and methanol (0.4 wt%), these concentrations falling within common range for Solar system comets.<ref>Template:Cite journal</ref> On 22 January 2015, NASA reported that, between June and August 2014, the comet released increasing amounts of water vapor, up to tenfold as much.<ref name="NASA-20150122"/> On 23 January 2015, the journal Science published a special issue of scientific studies related to the comet.<ref name="SCI-20150123"/>

Measurements carried out before PhilaeTemplate:'s batteries failed indicate that the dust layer could be as much as Template:Cvt thick. Beneath that is hard ice, or a mixture of ice and dust. Porosity appears to increase toward the center of the comet.<ref name="esa20141218"/>

The nucleus of Churyumov–Gerasimenko was found to have no magnetic field of its own after measurements were taken during PhilaeTemplate:'s descent and landing by its ROMAP instrument and RosettaTemplate:'s RPC-MAG instrument. This suggests that magnetism may not have played a role in the early formation of the Solar System, as had previously been hypothesized.<ref name="esa20150414"/><ref name="nature20150414"/>

The ALICE spectrograph on Rosetta determined that electrons (within Template:Cvt 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.<ref name="NASA-20150602"/><ref name="AA-20150602"/> Also, active pits, related to sinkhole collapses and possibly associated with outbursts are present on the comet.<ref name="NAT-20150702"/><ref name="AP-20150701"/>

Measurements by the COSAC and Ptolemy instruments on the PhilaeTemplate:'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.<ref name="wapo20150730"/><ref name="esa20150730"/><ref name="SCI-20150731"/> Astrobiologists Chandra Wickramasinghe and Max Wallis stated that some of the physical features detected on the comet's surface by Rosetta and Philae, such as its organic-rich crust, could be explained by the presence of extraterrestrial microorganisms.<ref name="TG-20150705"/><ref name="SN-20150706"/> Rosetta program scientists dismissed the claim as "pure speculation".<ref name="TT-20150706"/> Carbon-rich compounds are common in the Solar System. Neither Rosetta nor Philae is equipped to search for direct evidence of organisms.<ref name="TG-20150705"/> The only amino acid detected thus far on the comet is glycine, along with precursor molecules methylamine and ethylamine.<ref name="Altwegg 2016"/>

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 the insoluble organic matter in carbonaceous chondrite meteorites. Scientists think that the observed cometary carbonaceous solid matter could have the same origin as the meteoritic insoluble organic matter, but suffered less modification before or after being incorporated into the comet.<ref name="Fray 2016"/>

One of the most outstanding discoveries of the mission was the detection of large amounts of free molecular oxygen (Template:Chem2) gas surrounding the comet. Solar system models suggest the molecular oxygen should have disappeared by the time 67P was created, about 4.6 billion years ago in a violent and hot process that would have caused the oxygen to react with hydrogen and form water.<ref name="Bieler 2015"/><ref name="Howel 2015"/> Molecular oxygen has never before been detected in cometary comas. In situ measurements indicate that the Template:Chem2/Template:Chem2 ratio is isotropic in the coma and does not change systematically with heliocentric distance, suggesting that primordial Template:Chem2 was incorporated into the nucleus during the comet's formation.<ref name="Bieler 2015"/> This interpretation was challenged by the discovery that Template:Chem2 may be produced on the surface of the comet in water molecule collisions with silicates and other oxygen-containing materials.<ref name="Yao 2017"/> Detection of molecular nitrogen (Template:Chem2) in the comet suggests that its cometary grains formed in low-temperature conditions below Template:Cvt.<ref name="Rubin2015"/>

On 3 July 2018, researchers hypothesized that molecular oxygen might not be made on the surface of comet 67P in sufficient quantity, thus deepening the mystery of its origin.<ref name="Heritier2018"/><ref name="imperial20180703"/>

Future missions

CAESAR was a proposed sample-return mission aimed at returning to 67P/Churyumov–Gerasimenko, capturing regolith from the surface, and returning it to Earth.<ref name="nasa20171220"/><ref name="nytimes20171219"/> This mission was competing in NASA's New Frontiers mission 4 selection process, and was one of two finalists in the program.<ref name="ibtimes20171220"/> In June 2019, it was passed over in favor of Dragonfly.<ref name="nyt20190627"/><ref name="spnews20190627"/>

Gallery

A reconstruction of the nucleus's shape based on Hubble observations in 2003
As seen by the Very Large Telescope on 11 August 2014<ref name="esobs20140908"/>
As seen by Rosetta on 22 August 2014
As seen by Rosetta on 14 September 2014
As seen by Rosetta on 28 March 2015
As seen by Rosetta on 2 May 2015
As seen by Rosetta on 7 July 2015
Image showing ragged cliffs, 10 December 2014
CitationClass=web }}</ref>
Comet 67P/Churyumov–Gerasimenko in enhanced colour, as imaged by ESA's Rosetta spacecraft in 2015