911 research outputs found
Pebble accretion at the origin of water in Europa
Despite the fact that the observed gradient in water content among the
Galilean satellites is globally consistent with a formation in a circum-Jovian
disk on both sides of the snowline, the mechanisms that led to a low water mass
fraction in Europa () are not yet understood. Here, we present new
modeling results of solids transport in the circum-Jovian disk accounting for
aerodynamic drag, turbulent diffusion, surface temperature evolution and
sublimation of water ice. We find that the water mass fraction of pebbles
(e.g., solids with sizes of 10 -- 1 m) as they drift inward is globally
consistent with the current water content of the Galilean system. This opens
the possibility that each satellite could have formed through pebble accretion
within a delimited region whose boundaries were defined by the position of the
snowline. This further implies that the migration of the forming satellites was
tied to the evolution of the snowline so that Europa fully accreted from
partially dehydrated material in the region just inside of the snowline.Comment: Accepted for publication in Ap
First disk-resolved spectroscopy of (4) Vesta
Vesta, the second largest Main Belt asteroid, will be the first to be
explored in 2011 by NASA's Dawn mission. It is a dry, likely differentiated
body with spectrum suggesting that is has been resurfaced by basaltic lava
flows, not too different from the lunar maria.
Here we present the first disk-resolved spectroscopic observations of an
asteroid from the ground. We observed (4) Vesta with the ESO-VLT adaptive
optics equipped integral-field near-infrared spectrograph SINFONI, as part of
its science verification campaign. The highest spatial resolution of ~90 km on
Vesta's surface was obtained during excellent seeing conditions (0.5") in
October 2004.
We observe spectral variations across Vesta's surface that can be interpreted
as variations of either the pyroxene composition, or the effect of surface
aging. We compare Vesta's 2 micron absorption band to that of
howardite-eucrite-diogenite (HED) meteorites that are thought to originate from
Vesta, and establish particular links between specific regions and HED
subclasses. The overallcomposition is found to be mostly compatible with
howardite meteorites, although a small area around 180 deg. East longitude
could be attributed to a diogenite-rich spot. We finally focus our spectral
analysis on the characteristics of Vesta's bright and dark regions as seen from
Hubble Space Telescope's visible and Keck-II's near-infrared images.Comment: 13 pages, 11 figures, 3 table
Spectral properties of nine M-type asteroids
Reproduced with permission. Copyright ESO. Article published by EDP Sciences and available at http://www.aanda.org.International audienceAims. We present spectroscopic results for nine M-type asteroids (325 Heidelberga, 497 Iva, 558 Carmen, 687 Tinette, 766 Moguntia, 860 Ursina, 909 Ulla, 1280 Baillauda, and 1564 Srbija) in the 0.8−2.5 μm spectral region. One visible spectrum is also presented for the asteroid 497 Iva. These asteroids were observed during several runs between 2003 and 2007, and the main goal was to investigate the NIR spectral region of M-type asteroids. Methods. The data was obtained with SpeX/IRTF in Prism mode and Dolores/TNG in LR-B mode. Spectral analysis was performed by comparing the M-type spectra and the meteorite ones (χ2 approach) and the Modified Gaussian Model. Results. With one exception, the asteroids present positive slopes of the spectra, with no absorption features, in good agreement with the spectra of metallic meteorites. The analysis of the asteroid 766 Moguntia was done by means of χ2, MGM techniques, and the Shkuratov scattering law. We conclude that the mineralogy is dominated by olivine. Its NIR spectrum is similar to those of CO/CV meteorites
Rosetta Asteroid Candidates
AbstractThe new scenario of the Rosetta mission to comet 67/P Churyumov-Gerasimenko (launch on February 2004), includes as baseline the fly-by of one or two asteroids. Several asteroids are now possible fly-by candidates (single or double) within the available resources. Other candidates whose fly-bys require a larger Δv can be also considered if the Rosetta interplanetary orbit insertion will cost less Δv.All the up to date available information on the possible targets are discussed in this report
E-type asteroid (2867) Steins: flyby target for Rosetta
Reproduced with permission. Copyright ESO. Article published by EDP Sciences and available at http://www.aanda.org.International audienceAims. The mineralogy of the asteroid (2867) Steins was investigated in the framework of a ground-based science campaign dedicated to the future encounter with Rosetta spacecraft. Methods. Near-infrared (NIR) spectra of the asteroid in the 0.8−2.5 μm spectral range have been obtained with SpeX/IRTF in remoteobserving mode from Meudon, France, and Cambridge, MA, in December 2006 and in January and March 2007. A spectrum with a combined wavelength coverage from 0.4 to 2.5 μm was constructed using previously obtained visible data. To constrain the possible composition of the surface, we constructed a simple mixing model using a linear (areal) mix of three components obtained from the RELAB database. A space-weathering model was applied to the aubrite ALH-78113 spectrum. Results. The four new NIR spectra reveal no major absorption features. The best-fit model for the constructed visible-plus-NIR spectrum is represented by a mixture of 57% enstatite, 42% oldhamite, and 1% orthopyroxene. These results place Steins in a subdivision of the E-type class with objects like Angelina, Eger, and Nereus. This group is not sampled by the current collection of aubrite meteorites. Interestingly, the reddened aubrite spectrum also provides a good match to the Steins VNIR spectrum
Near infra-red spectroscopy of the asteroid 21 Lutetia. II. Rotationally resolved spectroscopy of the surface
Reproduced with permission. Copyright ESO. Article published by EDP Sciences and available at http://www.aanda.orgInternational audienceAims. In the framework of the ground-based science campaign dedicated to the encounter with the Rosetta spacecraft, the mineralogy of the asteroid (21) Lutetia was investigated. Methods. Near-infrared (NIR) spectra of the asteroid in the 0.8−2.5 μm spectral range were obtained with SpeX/IRTF in remote observing mode from Meudon, France in March and April 2006. We analysed these data together with previously acquired spectra - March 2003, August 2004. I-band relative photometric data obtained on 20 January 2006 using the 105 cm telescope from Pic du Midi, France has been used to build the ephemeris for physical observations. A χ2 test using meteorite spectra from the RELAB database was performed in order to find the best fit of complete visible + infrared (VNIR) spectra of Lutetia. Results. The new spectra reveal no absorption features. We find a clear spectral variation (slope), and a good correspondence between spectral variations and rotational phase. Two of the most different spectra correspond to two opposite sides of the asteroid (sub-Earth longitude difference around 180◦). For the neutral spectra a carbonaceous chondrite spectrum yields the best fit, while for those with a slightly positive slope the enstatitic chondrite spectra are the best analog. Based on the chosen subset of the meteorite samples, our analysis suggests a primitive, chondritic nature for (21) Lutetia. Differences in spectra are interpreted in terms of the coexistence of several lithologies on the surface where the aqueous alteration played an important role
Asteroid target selection for the new Rosetta mission baseline: 21 Lutetia and 2867 Steins
Reproduced with permission. Copyright ESO. Article published by EDP Sciences and available at http://www.aanda.org.International audienceThe new Rosetta mission baseline to the comet 67P/Churyumov-Gerasimenko includes two asteroid fly-bys. To help in target selection we studied all the candidates of all the possible scenarios. Observations have been carried out at ESO-NTT (La Silla, Chile), TNG (Canaries), and NASA-IRTF (Hawaii) telescopes, in order to determine the taxonomy of all the candidates. The asteroid targets were chosen after the spacecraft interplanetary orbit insertion manoeuvre, when the available total amount of ΔV was known. On the basis of our analysis and the available of ΔV, we recommended to the ESA ScienceWorking Group the asteroids 21 Lutetia and 2867 Steins as targets for the Rosetta mission. The nature of Lutetia is still controversial. Lutetia's spectral properties may be consistent with a composition similar to carbonaceous chondrite meteorites. The spectral properties of Steins suggest a more extensive thermal history. Steins may have a composition similar to relatively rare enstatite chondrite/achondrite meteorites
VLT/SPHERE observations and shape reconstruction of asteroid (6) Hebe
(6) Hebe is a large main-belt asteroid, accounting for about half a percent of the mass of the asteroid belt. Its spectral characteristics and close proximity to dynamical resonances within the main-belt (the 3:1 Kirkwood gap and the nu6 resonance) make it a probable parent body of the H-chondrites and IIE iron meteorites found on Earth.We present new AO images of Hebe obtained with the high-contrast imager SPHERE (Beuzit et al. 2008) as part of the science verification of the instrument. Hebe was observed close to its opposition date and throughout its rotation in order to derive its 3-D shape, and to allow a study of its surface craters. Our observations reveal impact zones that witness a severe collisional disruption for this asteroid. When combined to previous AO images and available lightcurves (both from the literature and from recent optical observations by our team), these new observations allow us to derive a reliable shape model using our KOALA algorithm (Carry et al. 2010). We further derive an estimate of Hebe's density based on its known astrometric mass
The remarkable surface homogeneity of the Dawn mission target (1) Ceres
Dwarf-planet (1) Ceres is one of the two targets, along with (4) Vesta, that
will be studied by the NASA Dawn spacecraft via imaging, visible and
near-infrared spectroscopy, and gamma-ray and neutron spectroscopy. While
Ceres' visible and near-infrared disk-integrated spectra have been well
characterized, little has been done about quantifying spectral variations over
the surface. Any spectral variation would give us insights on the geographical
variation of the composition and/or the surface age. The only work so far was
that of Rivkin & Volquardsen (2010, Icarus 206, 327) who reported
rotationally-resolved spectroscopic (disk-integrated) observations in the
2.2-4.0 {\mu}m range; their observations showed evidence for a relatively
uniform surface. Here, we report disk-resolved observations of Ceres with
SINFONI (ESO VLT) in the 1.17-1.32 {\mu}m and 1.45-2.35 {\mu}m wavelength
ranges. The observations were made under excellent seeing conditions (0.6"),
allowing us to reach a spatial resolution of ~75 km on Ceres' surface. We do
not find any spectral variation above a 3% level, suggesting a homogeneous
surface at our spatial resolution. Slight variations (about 2%) of the spectral
slope are detected, geographically correlated with the albedo markings reported
from the analysis of the HST and Keck disk-resolved images of Ceres (Li et al.,
2006, Icarus 182, 143; Carry et al., 2008, A&A 478, 235). Given the lack of
constraints on the surface composition of Ceres, however, we cannot assert the
causes of these variations.Comment: 8 pages, 5 figures, 2 tables, accepted for publication in Icaru
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