Rosetta: OSIRIS detects hints of ice in the comet’s neck

Located on the neck of comet 67P/Churyumov-Gerasimenko, the Hapi region displays a blueish reflectivity spectrum in OSIRIS color images.

March 13, 2015

The Hapi region on the neck of Rosetta’s comet 67P/Churyumov-Gerasimenko reflects red light less effectively than most other regions on the comet. It thus appears slightly blueish. The Hapi region is located between the comet’s two lobes and has in the past months proven to be particularly active and the source of spectacular jets of dust and gas. Scientists from the OSIRIS team are using images obtained with the color filters of Rosetta’s scientific imaging system to study the reflectivity properties of 67P’s surface. Their analyses confirm that the Hapi region is unique. Its bluish coloring might point to the presence of frozen water mixed intimately with the dust at the surface.

When seen with the human eye, comet 67P/Churyumov-Gerasimenko is grey – all over. With its color filters Rosetta’s scientific imaging system OSIRIS, however, can discern tiny differences in reflectivity. To this effect, scientists from the OSIRIS team image the same region on the comet’s surface using different color filters. If, for example, the region appears especially bright in one of these images, it reflects light of this wavelength especially well. 

“Even though the color variations on 67P’s surface are minute, they can give us important clues”, says OSIRIS Principal Investigator Holger Sierks from the Max Planck Institute for Solar System Research (MPS) in Germany. In a recent analysis performed by the OSIRIS team, the Hapi region clearly stands out from the rest of the comet: while most parts of 67P display a slightly reddish reflectivity spectrum as is common for cometary nuclei and other primitive bodies, the reflection of red light is somewhat lower in this region.

“We know that the reflectivity properties are closely correlated to the surface morphology”, says OSIRIS scientist Sonia Fornasier from the Paris Observatory. Where the smooth surface of the Hapi region gives way to the more rugged terrain of the surrounding areas, the reflectivity, too, changes. The scientists believe that Hapi’s special reflectivity properties hint at a higher abundance of frozen water at or near the surface. Earlier comet missions had observed similar behavior on comets 103P/Hartley 2 and 9P/Temple 1 and associated the bluish spectrum to the presence of frozen water. While OSIRIS can only study a limited number of spectral bands, Rosetta is equipped with other instruments such as VIRTIS than can unambiguously identify the spectral signature of water molecules in infrared reflection. “We are excited to see, whether our suspicion will be confirmed”, says Sierks.

The Hapi region differs from the rest of 67P’s surface in many respects. Not only is it much smoother, it is one of the main sources of activity in the Northern hemisphere. Early dust jets originated there. “During perihelion when 67P heats up significantly Hapi is hidden in Northern polar night. Outbound on the comet’s orbit, from March 2016, Hapi will receive solar heat again”, says Fornasier. “At this large distance from the Sun it will then be very cold. Hapi might therefore be a region that has been able to retain ices on its surface during past orbits around the Sun and has thus enough “fuel” left to create the fireworks of activity we have witnessed in the past months.”

Rosetta is an ESA mission with contributions from its member states and NASA. Rosetta's Philae lander is provided by a consortium led by DLR, MPS, CNES and ASI. Rosetta is the first mission in history to rendezvous with a comet, escort it as it orbits the Sun, and deploy a lander to its surface.

The scientific imaging system OSIRIS was built by a consortium led by the Max Planck Institute for Solar System Research (Germany) in collaboration with CISAS, University of Padova (Italy), the Laboratoire d'Astrophysique de Marseille (France), the Instituto de Astrofísica de Andalucia, CSIC (Spain), the Scientific Support Office of the European Space Agency (The Netherlands), the Instituto Nacional de Técnica Aeroespacial (Spain), the Universidad Politéchnica de Madrid (Spain), the Department of Physics and Astronomy of Uppsala University (Sweden), and the Institute of Computer and Network Engineering of the TU Braunschweig (Germany). OSIRIS was financially supported by the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), and Sweden (SNSB) and the ESA Technical Directorate.

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