Binary asteroid in Jupiter’s orbit
may be icy comet from solar
system’s earliest days
UC-Berkeley Press release
Contact: Robert Sanders
Berkeley — A bound pair of icy comets similar to the dirty snowballs circling outside the orbit of Neptune has been found lurking in the shadow of Jupiter.
Astronomers at the University of California, Berkeley, working with colleagues in France and at the Keck Telescope in Hawaii, have calculated the density of a known binary asteroid system that shares Jupiter’s orbit, and concluded that Patroclus and its companion probably are composed mostly of water ice covered by a patina of dirt.
Because dirty snowballs are thought to have formed in the outer reaches of the solar system, from which they are occasionally dislodged and end up looping closer to the sun as comets, the team suggests that the asteroid probably formed far from the sun. It most likely was captured in one of Jupiter’s Trojan points – two eddies where debris collects in Jupiter’s orbit – during a period when the inner solar system was intensely bombarded by comets, around 650 million years after the formation of the solar system.
If confirmed, this could mean that many or most of the probably thousands of Jupiter’s Trojan asteroids are dirty snowballs that originated much farther from the sun and at the same time as the objects now occupying the Kuiper Belt.
“It’s our suspicion that the Trojans are small Kuiper Belt objects,” said study leader Franck Marchis, a research astronomer at UC Berkeley.
Marchis and colleagues from the Institut de Mécanique Céleste et Calculs d’Éphémérides (IMCCE) at the Observatoire de Paris and from the W. M. Keck Observatory report their findings in the Feb. 2 issue of Nature.
The team’s conclusion adds support to a recent hypothesis about the evolution of the orbits of our solar system’s largest planets, Jupiter, Saturn, Uranus and Neptune, put forth by a group of researchers headed by Alessandro Morbidelli, a theoretical astronomer with the Conseil National de la Recherche Scientifique laboratory of the Observatoire de la Cote d’Azur, Nice, France.
In a Nature paper earlier this year, Morbidelli and colleagues proposed that icy comets would have been captured in Jupiter’s Trojan points during the early history of the solar system. According to their scenario, during the first few hundred million years after the birth of the solar system, the large gas planets orbited closer to the sun, enveloped in a cloud of billions of large asteroids called planetesimals, perhaps 100 kilometers (62 miles) in diameter or less. Interactions with these planetesimals caused the large gaseous planets to migrate outward until about 3.9 billion years ago, when Jupiter and Saturn entered resonant orbits and began tossing the planetesimals around like confetti, some of them leaving the solar system for good.
The bulk of the remaining planetesimals settled into orbits beyond Neptune – today’s Kuiper Belt and the source of short-period comets – but a small number were captured in the Trojan eddies of the giant planets, in particular Jupiter.
“This is the first time anyone has determined directly the density of a Trojan asteroid, and it supports the new scenario proposed by Morbidelli,” said coauthor Daniel Hestroffer, an astronomer at the IMCEE. “These asteroids would have been captured in the Trojan points at a time when the rocky planets were still forming, and this perturbation of the planetesimals about 650 million years after the birth of the solar system could have created the late bombardment of the moon and Mars.”
Though Marchis refers to the scenario as “a nice story,” he admits that more work needs to be done to provide support for it.
“We need to discover more binary Trojans and observe them to see if low density is a characteristic of all Trojans,” he said.
Trojan asteroids are those caught in the so-called Lagrange points of Jupiter’s orbit, located the same distance from Jupiter as Jupiter is from the sun – 5 astronomical units, or 465 million miles. These points, one leading and the other trailing Jupiter, are places were the gravitational attraction of the sun and Jupiter are balanced, allowing debris to collect like dust bunnies in the corner of a room. Hundreds of asteroids have been discovered in the leading (L4) and trailing (L5) points, each orbiting around that point as if in an eddy.
The asteroid 617 Patroclus, originally discovered at L5 and named in 1906, was found to have a companion in 2001, and so far is the only known Trojan binary. The discoverers were not able to estimate the orbit of the components because they had too few observations.
As experienced asteroid hunters, Marchis and his colleagues in August this year discovered the first triple asteroid system, 87 Sylvia, much closer to the sun in the main asteroid belt between Mars and Jupiter, and used a powerful 8-meter telescope of the European Southern Observatory’s Very Large Telescope in Chile to study the three objects. They were able to chart the orbits of the asteroids to estimate the density of Sylvia, from which they concluded it is a rubble-pile of loosely, packed rock.
The French and American team tried the same technique with the much more distant Patroclus, employing imaging data from the Keck II Laser Guide Star System at the W. M. Keck Observatory on Mauna Kea, which yields a sharp resolution impossible with any other ground-based telescope.
“Before, we could only look at objects near a bright reference star, limiting the use of adaptive optics to a small percentage of the heavens,” Marchis said. “Now, we can use adaptive optics to view almost any point on the sky.”
The laser guide star system uses a laser beam to excite sodium atoms within a small spot in the upper atmosphere. This artificial “star” is used to measure atmospheric turbulence, which is then removed by the movable mirrors of the Keck adaptive optics system.
With the system providing an unparalleled 58 milliarcsecond resolution, the Keck team made five observations in the infrared between November 2004 and July 2005. Marchis and his colleagues determined that the density of Patroclus and its companion, which are about the same size and circle around their center of mass every 4.3 days at a distance of 680 kilometers (423 miles), was very low: 0.8 grams per cubic centimeter, about one third that of rock and light enough to float in water. Assuming a rocky composition similar to that of Jupiter’s moons Callisto and Ganymede, the components of the system would have to be very loosely packed – about half empty space, an internal characteristic which is not expected for a same-size binary system, the researchers concluded.
The team suggests a more reasonable composition of water ice with only 15 percent open space, which makes these objects similar to comets and small Kuiper Belt objects, which have been determined to have densities less than water.
Marchis suspects that the binary system formed when a single large asteroid was torn asunder by the gravitational tug of Jupiter.
“The Patroclus system displays similar characteristics to the binary Near Earth Asteroids, which are believed to have formed during an encounter with a terrestrial planet by tidal splitting,” he said. “In the case of a Trojan asteroid, it is only when the work of our collaborators was published recently that we could suggest that this encounter was with Jupiter.”
Because in Homer’s Iliad, Patroclus was Achilles’ companion and a hero of the Trojan War, Achilles would have been an appropriate name for one of the two asteroids, which are about the same size. However, another asteroid already has the name Achilles, so Marchis and his collaborators proposed naming the smallest member of the binary system Menoetius, after the father of Patroclus. The Committee on Small Body Names of the International Astronomical Union has tentatively accepted the name. The asteroid designated Menoetius is about 112 kilometers (70 miles) in diameter, while Patroclus is about 122 kilometers (76 miles) wide.
In addition to Marchis, the team included astronomy professor Imke de Pater and postdoctoral fellow Michael H. Wong of UC Berkeley; Daniel Hestroffer, Pascal Descamps, Jérôme Berthier and Frédéric Vachier of the Institut de Mécanique Céleste et de Calculs des Éphémérides (IMCCE); and Antonin Bouchez, Randall Campbell, Jason Chin, Marcos van Dam, Scott Hartman, Erik Johansson, Robert Lafon, David Le Mignant, Paul Stomski, Doug Summers and Peter Wizinovich of the W. M. Keck Observatory.
This work was partially supported by the National Science Foundation Science and Technology Center for Adaptive Optics, and managed by the University of California at Santa Cruz under cooperative agreement No. AST-9876783. This material is partly based upon work supported by theNational Aeronautics and Space Administration issue through the Science Mission Directorate Research and Analysis Programs. Most of the data were obtained at the W. M. Keck observatory, which is operated as a scientific partnership between the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory and its AO system were made possible by the generous financial support of the W. M. Keck Foundation. Additional observations were obtained at theGemini Observatory (acquired through the Gemini Science Archive), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership.
The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
Fig.1: The asteroid 617 Patroclus and its companion are indicated by the green triangle in Jupiter’s trailing Lagrange point. The white dots indicate the position of the 10,000 known asteroids in our solar system with diameters greater than 10 kilometers. They cluster in the main asteroid belt between Mars and Jupiter, plus the two Lagrange points of Jupiter’s orbit.
(Credit: IMCCE-Observatoire de Paris)
Fig.2: 617 Patroclus observed with the Keck-10m LGS AO system. The observations of this faint object (mv~15.8) were made possible using the LGS system. An artificial star (with mv~11) is created at proximity of the target, exciting the thin sodium layer at an altitude of ~100 km using a dye laser. The asteroid itself was used for the tip-tilt analysi. These observations were taken on 28 May 2005 with the NIRC-2 infrared camera through the H, centred at 1.6 microns (a), and Kp, centred at 2.2 microns (b) broadband filters. The angular resolution is estimated to 0.058 arcsec, close to the diffraction limit of the telescope (indicated by the scale bar, 50mas). The angular separation on the two images is 150 mas, corresponding to 640 km, close to the maximum apparent separation of the components. (credit: F. Marchis et al., Nature)
Fig.3: The Keck-II Laser Guide Star system in operation on the top of Mauna Kea (credit: Sarah Anderson)