EPSC-DPS 2011/08: Hyperactive Hartley 2 has a split history
EPSC-DPS JOINT MEETING 2011 PRESS NOTICE
Ref. PN: EPSC11/08
The latest analysis of data from NASA’s Deep Impact spacecraft shows that comet 103P/Hartley 2 is hyperactive in terms of the material it spews out, compared to the other comets observed up close to date. The comet also shows surprising diversity – ice on the comet’s sunlit surface is found in patches that are isolated from areas of dust. In addition, one lobe of the dog-bone shaped comet may have lost much more of the primordial material from the formation of the comet than the other, suggesting that Hartley 2 was originally two comets that came together in a gentle collision. Mike A’Hearn and Lori Feaga will be presenting their findings at the EPSC-DPS Joint Meeting 2011 in Nantes, France.
Deep Impact made its closest encounter of Hartley 2 on 4 November 2010. Over the past year, the science team has been pouring over the data to gain a more detailed understanding of the processes that drive the comet’s activity.
“Hartley 2 works differently from Tempel 1, which was encountered by Deep Impact in 2005 and from Wild 2, which was observed by the Stardust mission. It ejects a huge amount of material for its size. Halley, which was observed by the Giotto mission lies somewhere in the middle of the spectrum of activity. Since the encounter, we have been able to dig deeper into the data and have provided more evidence of how ice and dust is released from the nucleus,” said A’Hearn, the Principal Investigator of Deep Impact’s mission extension, EPOXI.
Carbon dioxide gas, or dry ice, sublimates beneath the comet’s surface when it feels heat from the Sun and this fuels extensive jet activity on the comet. Much more carbon dioxide is escaping Hartley 2 than the other comets observed, including Tempel 1. The Deep Impact cameras and spectrometer have observed fragile chunks of water ice and dust being dragged from the nucleus with the escaping carbon dioxide into the comet’s atmosphere, or coma. The latest results are giving the team a better understanding of the nucleus and how the micrometre-sized grains of pure ice and centimetre sized dust particles are released from Hartley 2 into the coma. They have found that, despite the hyperactive release of material, both the ice and the volatiles within the dust are actually moving and subliming very slowly.
The team has found a large region of bright, rough terrain on the surface that is covered in water ice particles, a few hundredths of a millimetre in size. Through a combination of surface temperature analysis and the fact that the ice exists on the sunlit surface, they have deduced that these ice particles must be physically separate from the warm, dark dust and not intimately mixed.
Although inferred by the wealth of approach and departure data and preliminary mapping of the coma at closest approach, the team has also definitively reported that the larger lobe of Hartley 2’s nucleus currently has less carbon dioxide being released from it than the smaller lobe. This means that the volatile ices, primordial material from the formation of the comet located tens of centimetres deep into the nucleus, may be depleted in the larger lobe.
Lori Feaga, from the University of Maryland, says, “The heterogeneity between lobes is most likely due to compositional differences in the originally accreted material.”
“We are speculating that this means that the two lobes of the comet formed in different places in the Solar System. They came together in a gradual collision and the central part of the dog-bone was in-filled with dust and ice from the debris,” adds A’Hearn
From observations made from telescopes here on Earth, Deep Impact collaborators Matthew Knight and David Schleicher have shown that the grains are gradually shedding water and all the material is slowly moving away from the sun. This result complements the findings from the spacecraft team.
A’Hearn concludes, “All of these detailed findings put together, those from the spacecraft and supporting ground-based telescopes, may require us to rethink cometary origins.”
Launched in January 2005, the Deep Impact spacecraft smashed a probe into comet Tempel 1 on July 4th to see what kind of materials the comet was made of and how the surface would respond to a manmade impact. Once the successful primary mission was completed, a University of Maryland-led team of scientists proposed to fly the Deep Impact spacecraft to a second comet in order to characterize and directly compare two comets with one suite of instruments.
EPOXI, which is a combination of the names for the extended mission’s two components: the Extrasolar Planet Observations and Characterization (EPOCh), and the flyby of comet Hartley 2, called the Deep Impact Extended Investigation (DIXI), was approved. The mission scientists are continuing to dig deeper into the data to achieve the greatest science return for the ~120,000 images and spectra that the mission collected of Hartley 2.
NASA’s Jet Propulsion Laboratory, Pasadena, Calif., manages the EPOXI mission for NASA’s Science Mission Directorate, Washington. The University of Maryland, College Park, is home to the mission’s principal investigator, Michael A’Hearn and ten other members of the EPOXI science team. Drake Deming of NASA’s Goddard Space Flight Center, Greenbelt, Md., is the science lead for the mission’s extrasolar planet observations. The spacecraft was built for NASA by Ball Aerospace & Technologies Corp., Boulder, Colo.
A swarm of large chunks surrounding comet Hartley 2 was imaged with the Deep Impact spacecraft’s Medium Resolution Instrument. This clear filter image has been processed to enhance the visibility of the chunks. This processing saturates the comet nucleus and some of its nearby dust (lower right). The Sun is located to the right, and the spacecraft was at a distance of 807 km from the comet. (M. Kelley et al.)
On the inbound leg of the trip past comet Hartley 2, the Deep Impact spacecraft saw water ice on the surface of the comet. The presence of water ice is suggested in an enhanced color High Resolution Instrument (HRI) image, left panel, along the morning edge of the nucleus. The blue color is indicative of ice. In the middle HRI image, bright rough terrain can be seen. In the right panel, a map of the amount and location of water ice on the large lobe of the nucleus, estimated from spectral data, is overlaid on an HRI visible image to show the collocation of water ice with the bright rough terrain. Blue indicates ice concentrations while pink indicates a warm, dusty nucleus with no ice. Spectroscopic data at this resolution of the small lobe do not exist. (J. Sunshine et al.)
Distribution maps of the coma can be made from infrared scans. These HRI-IR maps of the near nucleus coma in the left panels, acquired during closest approach to the nucleus of Hartley 2, show an enhancement of carbon dioxide emanating from the sunward facing small lobe of the nucleus. The water vapour, however, has a different distribution implying a different source region and process. A half a rotation later, when the small lobe is pointing away from the Sun and the nucleus is no longer resolved in the HRI telescope (right panels), the carbon dioxide is still concentrated around the small lobe, and thus enhanced in the anti-sunward direction. In this larger field of view, the water is also enhanced away from the Sun, suggesting that water ice dragged out by the carbon dioxide is pushed away from the Sun by its radiation pressure and eventually sublimes. The Sun is to the right for all panels and the pixels in which the nucleus is located are black. (L. Feaga et al.)
The left panel shows that CN, a breakdown product of HCN and other molecules, is concentrated in the prominent jets of comet Hartley 2. Other breakdown products have a similar distribution. However, the middle panel shows that the distribution of OH, a breakdown product of water, is mostly tailward, i.e. away from the Sun. This implies that the release of water is decoupled from other gases and is almost certainly arising from nearly pure icy grains that are starting to drift tailward. The right panel shows the distribution of reflected blue light, which is also likely dominated by icy grains, to also be predominantly tailward. These ground-based data were collected by M. Knight & D. Schleicher in November 2010 from Lowell Observatory.
Department of Astronomy
University of Maryland
College Park, MD 20742
Lori M. Feaga
Department of Astronomy
University of Maryland
College Park, MD 20742