Since its arrival at comet 67P/Churyumov-Gerasimenko, the European Space Agencys Rosetta spacecraft has been surveying the surface and the environment of this curiously shaped body.
But for a long time, a portion of the nucleus — the dark, cold regions around the comets south pole — remained inaccessible to almost all instruments on the spacecraft.
Due to a combination of its double-lobed shape and the inclination of its rotation axis, Rosettas comet has a very peculiar seasonal pattern over its 6.5-year-long orbit. Seasons are distributed very unevenly between the two hemispheres. Each hemisphere comprise parts of both comet lobes and the neck.
For most of the comets orbit, the northern hemisphere experiences a very long summer, lasting over 5.5 years, while the southern hemisphere undergoes a long, dark and cold winter. However, a few months before the comet reaches perihelion — the closest point to the Sun along its orbit — the situation changes, and the southern hemisphere transitions to a brief and very hot summer.
When Rosetta arrived at 67P/C-G in August 2014, the comet was still experiencing its long summer in the northern hemisphere, and regions on the southern hemisphere received very little sunlight. Moreover, a large part of this hemisphere, close to the comets south pole, was in polar night and had been in total darkness for almost five years.
With no direct illumination from the Sun, these regions could not be imaged with Rosettas OSIRIS (the Optical, Spectroscopic, and Infrared Remote Imaging System) science camera, or its Visible, InfraRed and Thermal Imaging Spectrometer (VIRTIS). For the first several months after Rosettas arrival at the comet, only one instrument on the spacecraft could observe and characterize the cold southern pole of 67P/C-G: the Microwave Instrument for Rosetta Orbiter (MIRO).
In a paper accepted for publication in the journal Astronomy and Astrophysics, scientists report on the data collected by MIRO over these regions between August and October 2014.
We observed the dark side of the comet with MIRO on many occasions after Rosettas arrival at 67P/C-G, and these unique data are telling us something very intriguing about the material just below its surface, said Mathieu Choukroun from NASAs Jet Propulsion Laboratory (JPL), Pasadena, California, lead author of the study.
Observing the comets southern polar regions, Choukroun and colleagues found significant differences between the data collected with MIROs millimeter and submillimeter wavelength channels. These differences might point to the presence of large amounts of ice within the first few tens of centimeters below the surface of these regions.
Surprisingly, the thermal and electrical properties around the comets south pole are quite different than what is found elsewhere on the nucleus, said Choukroun. It appears that either the surface material or the material thats a few tens of centimeters below it is extremely transparent, and could consist mostly of water ice or carbon-dioxide ice.
The difference between the surface and subsurface composition of this part of the nucleus and that found elsewhere might originate in the comets peculiar cycle of seasons. One of the possible explanations is that water and other gases that were released during the comets previous perihelion, when the southern hemisphere was the most illuminated portion of the nucleus. The water condensed again and precipitated on the surface after the season changed and the southern hemisphere plunged again into its long and cold winter.
These are, however, preliminary results, because the analysis depends on the detailed shape of the nucleus. At the time the measurements were made, the shape of the dark, polar region was not known with great accuracy.
We plan to revisit the MIRO data using an updated version of the shape model, to verify these early results and refine the interpretation of the measurements, added Choukroun.
Rosetta scientists will be testing these and other possible scenarios using data that were collected in the subsequent months, leading to the comets perihelion, which took place on Aug. 13, 2015 and beyond.
In May 2015, the seasons changed on 67P/C-G and the brief, hot southern summer, which will last until early 2016, began. As the formerly dark southern polar regions started to receive more sunlight, it has been possible to observe them with other instruments on Rosetta, and the combination of all data might eventually disclose the origin of their curious composition.
In the past few months, Rosetta has flown over the southern polar regions on several occasions, starting to collect data from this part of the comet after summer began there, said Matt Taylor, ESA Rosetta project scientist. At the beginning of the southern summer, we had a paucity of observations in these regions as Rosettas trajectory focused on the northern hemisphere due to ongoing communication with the lander, Philae. However, closer to perihelion we were able to begin observing the south.
Rosetta is currently on an excursion out to about 930 miles (1,500 kilometers) from the nucleus to study the comets environment at large. But the spacecraft will soon come closer to the comet, focusing on full orbits to compare the northern and southern hemispheres, as well as some slower passes in the south to maximize observations there. In addition, as activity will start to wane later this year, the team hopes to get closer to the nucleus and gain higher-resolution observations of the surface.
First, we observed these dark regions with MIRO, the only instrument able to do so at the time, and we tried to interpret these unique data. Now, as these regions became warmer and brighter around perihelion, we can observe them with other instruments, too.
Mark Hofstadter, MIRO principal investigator at JPL, adds, We hope that, by combining data from all these instruments, we will be able to confirm whether or not the south pole had a different composition and whether or not it is changing seasonally.
The MIRO instrument is a small, lightweight spectrometer that can map the abundance, temperature and velocity of cometary water vapor and other molecules that the nucleus releases. It can also measure the temperature up to about one inch (three centimeters) below the surface of the comets nucleus. One reason the subsurface temperature is important is that the observed gases likely come from sublimating ices beneath the surface. By combining information on the gas and the subsurface, MIRO is able to study this process in detail.
Comets are time capsules containing primitive material left over from the epoch when the Sun and its planets formed. Rosetta is the first spacecraft to witness at close proximity how a comet changes as it is subjected to the increasing intensity of the suns radiation. Observations will help scientists learn more about the origin and evolution of our solar system and the role comets may have played in the formation of planets.
Reference: Dark Side of 67P/Churyumov-Gerasimenko in Aug-Oct 2014. MIRO/Rosetta Continuum Observations of Polar Night in the Southern Regions, M. Choukroun et al., 2015, to appear in Astronomy & Astrophysics [http://dx.doi.org/10.1051/0004-6361/201526181].
Rosetta is an ESA mission with contributions from its member states and NASA. Rosettas Philae lander is provided by a consortium led by the German Aerospace Center, Cologne; Max Planck Institute for Solar System Research, Gottingen; French National Space Agency, Paris; and the Italian Space Agency, Rome. JPL, Pasadena, California, a division of the California Institute of Technology in Pasadena, manages the U.S. contribution of the Rosetta mission for NASAs Science Mission Directorate in Washington. JPL also built the MIRO and hosts its principal investigator, Mark Hofstadter. The Southwest Research Institute (San Antonio and Boulder, Colorado), developed the Rosetta orbiters IES and Alice instruments and hosts their principal investigators, James Burch (IES) and Alan Stern (Alice).
More information on the U.S. instruments aboard Rosetta: http://rosetta.jpl.nasa.gov
More information about Rosetta: http://www.esa.int/rosetta
