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Berkeley, California – February 2, 2006:
Astronomers have used the
Keck II Laser Guide Star
adaptive optics system to determine 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 the University of California, Berkeley. Marchis and colleagues from the
Institut de Mécanique Céleste et Calculs d'Éphémérides (IMCCE)
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 Côte d'Azur,
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.
The binary Trojan asteroid Patroclus, observed with the Keck II AO Laser Guide Star system.
This observation was taken on 28 May 2005 with the NIRC-2 infrared camera through the Kp (2.2µm) broadband filter. The angular resolution is estimated to be 0.058 arcsec.
The angular separation on the two images is 150 mas, corresponding to 640 km, close to the maximum apparent separation of the components.
Image: Franck Marchis et al., Nature
"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
"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. 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 the sharpest resolution possible 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.
F. Marchis, D. Hestroffer, P. Descamps, J. Berthier, A.H. Bouchez, R.D. Campbell,
J.C.Y. Chin, M.A. van Dam, S.K. Hartman, E.M. Johansson, R.E. Lafon, D. Le Mignant,
I. de Pater, P.J. Stomski, D.M. Summers, F. Vachier, P.L. Wizinovich and M.H. Wong,
"A low density of 0.8 g cm–3 for the Trojan binary asteroid 617 Patroclus," Nature 439, 565–567 (2006)
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