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Getting to know Rosetta's comet

The spacecraft is revealing Comet 67P/Churyumov-Gerasimenko as having a remarkable array of surface features and with many processes contributing to its activity, painting a complex picture of its evolution.
RELATED TOPICS: SOLAR SYSTEM | COMETS | COMET 67P | ROSETTA
Comet67P_8km
A section of the smaller of Comet 67P/Churyumov–Gerasimenko’s two lobes as seen through Rosetta’s narrow-angle camera from a distance of about 5 miles (8 kilometers) to the surface October 14, 2014.
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
In a special edition of the journal Science, initial results are presented from seven of Rosetta’s 11 science instruments based on measurements made during the approach to and soon after arriving at Comet 67P/Churyumov–Gerasimenko in August 2014.

The familiar shape of the dual-lobed comet has now had many of its vital statistics measured: the small lobe measures 1.6 by 1.4 by 1.1 miles (2.6 by 2.3 by 1.8 kilometers) and the large lobe 2.5 by 2.0 by 1.1 miles (4.1 by 3.3 by 1.8 km). The total volume of the comet is 5.1 cubic miles (21.4 km3), and the Radio Science Instrument has measured its mass to be 10 billion tons, yielding a density of 29 pounds per cubic foot (470 kg/m3).
Comet67P_maps
The 19 regions identified on Comet 67P/Churyumov–Gerasimenko are separated by distinct geomorphological boundaries. Following the ancient Egyptian theme of the Rosetta mission, they are named for Egyptian deities. They are grouped according to the type of terrain dominant within each region. Five basic categories of terrain type have been determined: dust-covered (Ma’at, Ash and Babi); brittle materials with pits and circular structures (Seth); large-scale depressions (Hatmehit, Nut and Aten); smooth terrains (Hapi, Imhotep and Anubis), and exposed, more consolidated (‘rock-like’) surfaces (Maftet, Bastet, Serqet, Hathor, Anuket, Khepry, Aker, Atum and Apis).
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

By assuming an overall composition dominated by water ice and dust with a density of 90–125 pounds per cubic foot (1,500–2,000 kg/m3), the Rosetta scientists show that the comet has a very high porosity of 70–80 percent, with the interior structure likely comprising weakly bonded ice-dust clumps with small void spaces between them.

The OSIRIS scientific camera has imaged some 70 percent of the surface to date; the remaining unseen area lies in the southern hemisphere that has not yet been fully illuminated since Rosetta’s arrival.

The scientists have so far identified 19 regions separated by distinct boundaries, and following the ancient Egyptian theme of the Rosetta mission, these regions are named for Egyptian deities and are grouped according to the type of terrain dominant within.

Five basic — but diverse — categories of terrain type have been determined: dust-covered; brittle materials with pits and circular structures; large-scale depressions; smooth terrains; and exposed more consolidated ("rock-like") surfaces.

Comet67P_active_pit
Active pit detected in Seth region of Comet 67P/Churyumov–Gerasimenko. Enhancing the contrast (right) reveals fine structures in the shadow of the pit, interpreted as jet-like features rising from the pit.
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
Comet67P_wind
Features in the Hapi region show evidence of local gas-driven transport producing dune-like ripples (left) and boulders with ‘wind-tails’ (right) — where the boulder has acted as a natural obstacle to the direction of the gas flow, creating a streak of material ‘downwind’ of it.
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
Much of the northern hemisphere is covered in dust. As the comet is heated, ice turns directly into gas that escapes to form the atmosphere or coma. Dust is dragged along with the gas at slower speeds, and particles that are not traveling fast enough to overcome the weak gravity fall back to the surface instead.

Some sources of discrete jets of activity also have been identified. While a significant proportion of activity emanates from the smooth neck region, jets also have been spotted rising from pits.     

The gases that escape from the surface also have been seen to play an important role in transporting dust across the surface, producing dune-like ripples and boulders with "wind-tails" — the boulders act as natural obstacles to the direction of the gas flow, creating streaks of material "downwind" of them.

The dusty covering of 67P may be several meters thick in places, and measurements of the surface and subsurface temperature by the Microwave Instrument on the Rosetta Orbiter (MIRO) suggest that the dust plays a key role in insulating the comet interior, helping protect the ices thought to exist below the surface.
Comet67P_alcove
Local bright spots, less than 33 feet (10 meters) across (labeled) and seen in an alcove in the Hathor region are compositionally distinct from the surrounding terrain.
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
Comet67P_crack
OSIRIS images of Comet 67P/Churyumov–Gerasimenko showing the details of a 0.3-mile-long (500 meters) crack running through the Hapi region. A context image showing the smooth, boulder-strewn Hapi region and the Hathor cliff face to the right is shown in the top left panel. The bottom-left panel indicates the crack extending across Hapi and beyond. The right panel shows the crack where it leaves Hapi and extends into Anuket, with Seth at the uppermost left and Hapi in the lower left.
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
Comet67P_goosebumps
Close-ups of a curious surface texture nicknamed "goosebumps." The characteristic scale of all the bumps seen on Comet 67P/Churyumov–Gerasimenko by the OSIRIS narrow-angle camera is approximately 10 feet (3 meters), extending over regions greater than 325 feet (100m). They are seen on very steep slopes and on exposed cliff faces, but their formation mechanism is yet to be explained.
ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
Small patches of ice also may be present on the surface. At scales of 50–80 feet (15–25 meters), Rosetta’s Visible, InfraRed and Thermal Imaging Spectrometer (VIRTIS) finds the surface to be compositionally very homogenous and dominated by dust and carbon-rich molecules, but largely devoid of ice. But smaller, bright areas seen in images are likely to be ice-rich. Typically, they are associated with exposed surfaces or debris piles where collapse of weaker material has occurred, uncovering fresher material.

On larger scales, many of the exposed cliff walls are covered in randomly oriented fractures. Their formation is linked to the rapid heating–cooling cycles that are experienced over the course of the comet’s 12.4-hour day and over its 6.5-year elliptical orbit around the Sun. One prominent and intriguing feature is a 0.3-mile-long (500m) crack seen roughly parallel to the neck between the two lobes, although it is not yet known if it results from stresses in this region.

Some very steep regions of the exposed cliff faces are textured on scales of roughly 10 feet (3m) with features that have been nicknamed "goosebumps." Their origin is yet to be explained, but their characteristic size may yield clues as to the processes at work when the comet formed.

And on the very largest scale, the origin of the comet’s overall double-lobed shape remains a mystery. The two parts seem very similar compositionally, potentially favoring the erosion of a larger single body. But the current data cannot yet rule out the alternative scenario: Two separate comets formed in the same part of the solar system and then merged together at a later date.

This key question will be studied further over the coming year as Rosetta accompanies the comet around the Sun.

How to grow an atmosphere
Their closest approach to the Sun occurs August 13 at a distance of 116 million miles (186 million km), between the orbits of Earth and Mars. As the comet continues to move closer to the Sun, an important focus for Rosetta’s instruments is to monitor the development of the comet’s activity, in terms of the amount and composition of gas and dust emitted by the nucleus to form the coma.

Images from the scientific and navigation cameras have shown an increase in the amount of dust flowing away from the comet over the past six months, and MIRO showed a general rise in the comet’s global water vapor production rate, from 1.3 cups (0.3 liters) per second in early June 2014 to 5.1 cups (1.2 liters) per second by late August. MIRO also found that a substantial portion of the water seen during this phase originated from the comet’s neck.

Water is accompanied by other outgassing species, including carbon monoxide and carbon dioxide. The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) is finding large fluctuations in the composition of the coma, representing daily and perhaps seasonal variations in the major outgassing species. Water is typically the dominant outgassing molecule, but not always.

By combining measurements from MIRO, ROSINA, and GIADA (Rosetta’s Grain Impact Analyzer and Dust Accumulator) taken between July and September, the Rosetta scientists have made a first estimate of the comet’s dust-to-gas ratio, with around four times as much mass in dust being emitted than in gas, averaged over the sunlit nucleus surface.

However, this value is expected to change once the comet warms up further and ice grains — rather than pure dust grains — are ejected from the surface.

GIADA also has been tracking the movement of dust grains around the comet, and, together with images from OSIRIS, two distinct populations of dust grains have been identified. One set is outflowing and is detected close to the spacecraft, while the other family is orbiting the comet no closer than 80 miles (130km) from the spacecraft.

It is thought that the more distant grains are left over from the comet’s last closest approach to the Sun. As 67P moved away from the Sun, the gas flow from the comet decreased and was no longer able to perturb the bound orbits. But as the gas production rate increases again over the coming months, it is expected that this bound cloud will dissipate. However, Rosetta will only be able to confirm this when it is farther away from the comet again — it is currently in a 20-mile (30km) orbit.

As the gas–dust coma continues to grow, interactions with charged particles of the solar wind and with the Sun’s ultraviolet light will lead to the development of the comet’s ionosphere and, eventually, its magnetosphere. The Rosetta Plasma Consortium (RPC) instruments have been studying the gradual evolution of these components close to the comet.

“Rosetta is essentially living with the comet as it moves towards the Sun along its orbit, learning how its behavior changes on a daily basis and, over longer timescales, how its activity increases, how its surface may evolve, and how it interacts with the solar wind,” said Matt Taylor, ESA’s Rosetta project scientist.

“We have already learned a lot in the few months we have been alongside the comet, but as more and more data are collected and analyzed from this close study of the comet, we hope to answer many key questions about its origin and evolution.”
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