J. Veverka

Cornell University, New York City, NY, United States

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Publications (490)2013.3 Total impact

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    ABSTRACT: Among the many Cassini ISS (Imaging Science Subsystem) images of Enceladus are a few severely-underexposed, motion-blurred images that were acquired on “boresight-drag” events on the closest flybys. During boresight-drags, ISS is statically aimed at a point that intercepts the predicted path of Enceladus’ across the sky. The ISS Narrow angle (NAC) and Wide Angle (WAC) cameras are repeatedly triggered together in hope of serendipitously capturing a close-up “BOTSIM” image-pair of the body as it passes. Because the events are so fast, the surface footprints and lighting geometry cannot be predicted in advance - a cascade of images are just quickly shuttered at the minimum 5 msec exposure. On each of four boresight-drags, surface images were captured. However, the two most recent (image-pair W/N1669812043 in November 2010 and W/N1713106405 in April 2012, respectively) were poorly illuminated -- three of four images only in Saturnshine. Despite their poor signal quality, they are rare images of Enceladus’ surface obtained with spatial resolutions better than a few meters/pixel. Careful use of Fourier filtering and spatial reconstruction techniques was needed to eliminate image noise and residual electronic banding that was not removed during routine radiometric calibration of the images. Fourier motion debluring techniques were then applied to correct for significant motion smear. Images W/N1669812043 (55.1°N, 20.2°W) are in old cratered terrain, inside a prominent 23 km sized impact crater along the rise of its updomed floor. They show a system of parallel ~250m wide mesas trending around the dome’s circumference. Smooth detritus inundates mesas and valleys near the dome summit and the mesa surfaces are otherwise mantled with regolith that is finely cratered down to the ~2 m/pixel NAC resolution limit. W/N1713106405 (66.9°S, 29.5°W) show the chaotically fractured margin of the active South Polar Terrain - an area divided by parallel ridges and troughs with relatively smooth flanks and valley floors. Quasi-linear arrangements of ice-blocks, each block tens of meters or smaller, are found mostly near ridge-tops.
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    ABSTRACT: More than a dozen small (<150 km mean radius) satellites occupy distinct dynamical positions extending from within Saturn's classical rings to the orbit of Dione. The Cassini mission has gradually accumulated image and spectral coverage of these objects to the point where some generalizations on surface morphology may be made. Objects in different dynamical niches have different surface morphologies. Satellites within the main rings display equatorial ridges. The F-ring shepherding satellites show structural forms and heavily cratered surfaces. The co-orbitals Janus and Epimetheus are the most lunar-like of the small satellites. Satellites occupying libration zones (Trojan satellites) have deep covering of debris subject to downslope transport. Small satellites embedded in ring arcs are distinctively smooth ellipsoids that are unique among small, well-observed Solar System bodies and are probably relaxed, effectively fluid equilibrium shapes indicative of mean densities of about 300 kg m‑3.
    Icarus 09/2013; 226:999-1019. · 3.16 Impact Factor
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    ABSTRACT: a b s t r a c t The nucleus of comet Tempel 1 has been investigated at close range during two spacecraft missions sep-arated by one comet orbit of the Sun, 5½ years. The combined imaging covers $70% of the surface of this object which has a mean radius of 2.83 ± 0.1 km. The surface can be divided into two terrain types: rough, pitted terrain and smoother regions of varying local topography. The rough surface has round depressions from resolution limits ($10 m/pixel) up to $1 km across, spanning forms from crisp steep-walled pits, to subtle albedo rings, to topographic rings, with all ranges of morphologic gradation. Three gravitationally low regions of the comet have smoother terrain, parts of which appear to be deposits from minimally modified flows, with other parts likely to be heavily eroded portions of multiple layer piles. Changes observed between the two missions are primarily due to backwasting of scarps bounding one of these probable flow deposits. This style of erosion is also suggested by remnant mesa forms in other areas of smoother terrain. The two distinct terrains suggest either an evolutionary change in processes, topo-graphically-controlled processes, or a continuing interaction of erosion and deposition.
    Icarus 02/2013; 222:453-466. · 3.16 Impact Factor
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    ABSTRACT: a b s t r a c t We present results from our study of the Stardust-NExT NAVCAM images of Comet 9P/Tempel 1, in which we analyze the dust coma and derive the locations and directions of 11 isolated jets detected around clos-est approach. Seven of the jets form a cluster that is associated with terraced terrain near the equator. Other jets arise from the nightside of the nucleus, having been in darkness for as long as 4 h, indicating that thermal lags continue to drive activity long after sunset. We compare the coma features observed here to those seen during the Deep Impact encounter on the previous apparition, and argue that much of the isolated jet activity is associated with steep slopes and the edges of smooth areas. We estimate that the cluster of jets produces 7–20% of the total dust in the coma, indicating that isolated sources play a significant role in the comet's activity. We measured an average dust production rate A(a)fq = 42 ± 6 cm at an approach phase angle of 79°, corresponding to a dust mass loss of approximately 264 kg s À1 . Our analysis also indicates that the Stardust-NExT spacecraft did not pass through any dust jets during the flyby.
    Icarus 02/2013; 222:540-549. · 3.16 Impact Factor
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    ABSTRACT: The Stardust-NExT (SdN) mission returned to Comet 9P/Tempel-1 and viewed the site of the Deep Impact (DI) collision just over one comet year later. Comparisons between pre-impact images from the ITS camera on the DI probe and SdN images reveal a 50 m-diameter crater surrounded by a low rim about 180 m in diameter. The removal of a small mound uprange (but offset from the trajectory) from the impact site can be related to changes in the evolution of ejecta. A narrow (6°) gap in the ejecta curtain downrange indicates that a ridge extending from the impact-facing scarp downrange interrupted the final stages of cratering in one small region. Together, these observations indicate that the DI excavation crater diameter was about 200 m (±20 m), a value consistent with the ejected mass derived from Earth- and space-based observations with the assumption that this mass represents only 10–20% of the total ejected mass. As a result, the DI crater visible today is consistent with either a larger transient crater, which collapsed, or a central crater of a nested crater resembling an inverted sombrero. The latter alternative would be expected from a layered target: a loose particulate surface about 1–2 m deep over a slightly more competent substrate.
    Icarus 02/2013; 222(2):502–515. · 3.16 Impact Factor
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    ABSTRACT: a b s t r a c t On February 14, 2011 Stardust-NExT (SN) flew by Comet Tempel 1, the target of the Deep Impact (DI) mission in 2005, obtaining dust measurements and high-resolution images of areas surrounding the 2005 impact site, and extending image coverage to almost two thirds of the nucleus surface. The nucleus has an average radius of 2.83 ± 0.1 km and a uniform geometric albedo of about 6% at visible wavelengths. Local elevation differences on the nucleus reach up to 830 m. At the time of encounter the spin rate was 213° per day (period = 40.6 h) and the comet was producing some 130 kg of dust per second. Some 30% of the nucleus is covered by smooth flow-like deposits and related materials, restricted to gravitational lows. This distribution is consistent with the view that the smooth areas represent material erupted from the subsurface and date from a time after the nucleus achieved its current shape. It is possible that some of these eruptions occurred after 1609 when the comet's perihelion distance decreased from 3.5 AU to the current 1.5 AU. Much of the surface displays evidence of layering: some related to the smooth flows and some possibly dating back to the accretion of the nucleus. Pitted terrain covers approximately half the nucleus surface. The pits range up to 850 m in diameter. Due to their large number, they are unlikely to be impact scars: rather they probably result from volatile outbursts and sublimational erosion. The DI impact site shows a subdued depression some 50 m in diameter implying surface properties similar to those of dry, loose snow. It is possible that the 50-m depression is all that remains of an initially larger crater. In the region of overlapping DI and SN coverage most of the surface remained unchanged between 2005 and 2011 in albedo, photometric properties and morphology. Significant changes took place only along the edges of a prominent smooth flow estimated to be 10–15 m thick, the margins of which receded in places by up to 50 m. Coma and jet activity were lower in 2011 than in 2005. Most of the jets observed during the SN flyby can be traced back to an apparently eroding terraced scarp. The dust instruments detected bursts of impacts consistent with a process by which larger aggregates of material emitted from the nucleus subsequently fragment into smaller particles within the coma.
    Icarus 02/2013; 222:424-435. · 3.16 Impact Factor
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    ABSTRACT: a b s t r a c t Observations from the second encounter of Comet 9P/Tempel 1 by the Stardust-NExT spacecraft provide an improved shape model and rotational pole for the nucleus (Thomas, P.C. et al. [2012]. Icarus 222, 453– 466) that allows us to greatly improve our knowledge of its rotational evolution beyond that outlined earlier in Belton et al. (Belton, M.J.S. et al. [2011]. Icarus 213, 345–368). Model light curves are shown to fit observations at both perihelia with a single pole direction indicating that polar precession during a single perihelion passage is small. We show that the rotational phasing associated with observations taken far from perihelion in the previous work was incorrectly assessed by approximately half a cycle leading us to a significant reassessment of the evolution of the non-gravitational torques acting on the nucleus. We present an updated spin rate profile (torque model) for the 2005 perihelion passage and show that retardation of the spin rate well before perihelion is no longer a required feature. With the exception of the spin rate before the 2000 perihelion passage, the evolution of rotational rates through the three most recent perihelion passages is largely unaffected as is the prediction of the rotational phase of the comet's nucleus at the Stardust-NExT near-perihelion encounter. We find a spin rate of 209.4 ± 0.01°/d likely applies in the quiescent period before the 2000 perihelion, a 0.2% change, and that the rotational period shortened by 12.3 ± 0.2 min during the 2000 perihelion passage. We present an analysis of Stardust-NExT time-series photometry that yields a spin rate near 213.3 ± 0.8°/d at the time of encounter. An application of the 2005 torque model suggests that, while roughly similar, the torques were probably weaker during the 2011 perihelion passage.
    Icarus 02/2013; 222:516-525. · 3.16 Impact Factor
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    ABSTRACT: a b s t r a c t The photometric properties of the nucleus of Comet 9P/Tempel 1 as modeled from the Stardust-NExT images agree with those reported by Li et al. from Deep Impact images. No signifi-cant changes are detectable by comparing the two image-sets taken one comet year apart. The overall photometric variations on the $70% of the surface of Tempel 1 observed by Deep Impact and Stardust-NExT are small, with albedo variations of ±10% full-width-at-half-maximum and non-detectable variations in phase function and surface roughness. Some bright surface albedo features visible in the outbound images have an albedo about 25% higher than that of surrounding area. No bright albedo features similar to those ice patches reported by Sunshine et al. (Sunshine, J.M., et al. [2006]. Science 311, 1453–1455) are seen on the outbound side, which was not imaged by DI. The similar global photo-metric properties among cometary nuclei may indicate that these properties are dominated by cometary activity that results in constant resurfacing on comets. Tiny amounts of ice concentration on their surface can significantly change the local photometric properties.
    Icarus 02/2013; 222:467-476. · 3.16 Impact Factor
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    ABSTRACT: We report detailed studies of the photometric properties of two cometary nuclei, 103P/Hartley 2 and 9P/Tempel 1, from DIXI flyby and Stardust-NExT flyby, respective, and the comparative studies of cometary nucleus photometry.
    LPI Contributions. 05/2012;
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    ABSTRACT: An overview of the discoveries and results made by the Stardust-NExT Science Team at the second encounter with comet 9P/Tempel 1 will be presented.
    LPI Contributions. 05/2012;
  • P. H. Schultz, B. Hermalyn, J. Veverka
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    ABSTRACT: The Stardust-NExT mission imaged the impact crater formed by the DI impact probe. The size of the crater is estimated to be 150 m to 200 m in diameter based on the observed crater and disruption of ejecta as seen in images from the DI flyby in 2005.
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    ABSTRACT: On 14 February 2011, the Stardust spacecraft performed its second cometary flyby, following the successful completion of primary mission to return coma samples from comet 81P/Wild 2. Stardust NExT passed within 200 km of the nucleus of comet 9P/Tempel 1, first visited by the Deep Impact spacecraft in 2005, providing an opportunity to make in-situ measurements of a second cometary coma with the same dust detection instruments. We present new results from the Dust Flux Monitor Instrument at the Tempel 1 flyby which detected bursts of impacts consistent with measurements at Wild 2, interpreted as the fragmentation of larger aggregates of material emitted from the nucleus into smaller particles within the coma.
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    ABSTRACT: On February 14, 2011 Stardust-NExT flew by Comet Tempel 1, the target of the Deep Impact mission in 2005, obtaining dust measurements and highresolution images of areas surrounding the 2005 impact site, and extending coverage to almost two thirds of the nucleus surface. No large-scale morphologic or photometric changes have occurred in the region of common coverage during the past six years. The most significant changes took place along the edges of a prominent smooth, flow-like feature, the margins of which receded in places by up to 50 meters. The amount of material removed is sufficient to account for about a percent of the estimated mass loss of the comet per perihelion passage. The DI impact site shows a subdued impact scar some 50 meters in diameter implying surface properties similar to those of dry, loose snow. Smooth areas cover about half of the newly imaged face of the comet. On the nucleus smooth regions are restricted to gravitational lows, consistent with the view that they originated from eruptions onto the surface and date from a time after the nucleus had achieved its present shape. Much of the surface of the comet displays evidence of pervasive layering. Two types of layers may be involved: some related to the smooth flows and others possibly dating back to the accretion of the nucleus. Coma and jet activity were lower in 2011 than in 2005. As was the case at the Wild 2 flyby in 2004, the dust instruments detected bursts of impacts consistent with a process by which larger aggregates of material emitted from the nucleus fragment into smaller particles within the coma.
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    ABSTRACT: New data obtained during the Stardust-NExT mission encounter has led to a substantial increase in the accuracy of the spin pole determination and shape model of the nucleus of comet 9P/Tempel 1. This has allowed improved determination of the locations of the mini-outbursts [1] that were discovered, but not imaged, around the Deep Impact mission encounter. The expanded mapping of the surface accomplished by Stardust-NExT includes high-resolution (~20 m/pixel) coverage of one of these areas under good lighting conditions thus providing views of candidate features caused by outburst eruptions and, possibly, a surface feature associated with the pre-eruption state. Plausible candidates for post-eruption features, located within 10 of the nominal location, are several irregularly shaped, fresh looking, depressions with central peaks. Also seen in the same region are two relatively smooth positive elevation features that we postulate may be associated with the pre-eruptive state. We compare these features to the full range of depression morphologies seen elsewhere on the imaged surface and discuss the possibility that most of the depressions seen on the surface were caused by outburst activity and subsequently eroded by sublimation. The mechanism responsible for outburst activity proposed earlier by Belton and Melosh [2] is briefly discussed in light of these new findings.
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    ABSTRACT: Tectonic shear along tiger stripes and other fractures at the South Pole of Enceladus is a key mechanism in current theories about active cryovolcanism and the tectonic evolution of the South Polar Terrain (SPT) region. Frictional heating of tiger stripe faults has been proposed to provide energy to drive cryovolcanic venting [1]. Tidal flexing of Enceladus's lithosphere, which has been proposed to control periodic opening and closing of volcanic fissures [2], results in oscillating stresses which, when resolved along tiger stripes, have both normal and shear components. The efficacy of frictional heating and strike-slip motion varies with the compressive or extensional intensity of the resolved normal stress component. Transpression is a state of stress that occurs when the surface experiences simultaneous compression and shear, while transtension occurs when it experiences simultaneous tension and shear. Significant lateral displacements along strike are expected to accompany shear failure in the tiger stripes [3], and large lateral offsets can accumulate over time due to the process of "tidal walking" [4] in which alternate periods of transtension and transpression on each tidal half-cycle provides the means by which one side of the rift can progressively ratchet laterally from the other. The identification and measurement of shear indicators along South Polar fractures may provide critical constraints on the thickness of Enceladus' lithosphere [5] and its possible librational history [6]. Transpression and transtension may also have been important in tectonism related to non-synchronous rotation [7,8]. In this study, we extend our earlier work [9,10] to identify and analyze geomorphologic indicators of transtension and transpression within tectonic features of the active SPT region on Enceladus. In addition to numerous strike-slip offsets visible along fractures, our Rosetta stone for interpreting these geomorphologic indicators is a prominent tectonic stepover structure at the distal ends of the tiger stripes on the Saturn-facing hemisphere (Fig. 1). Near Damascus Sulcus, the stepover features a (transtensional) releasing bend that is identified with a prominent negative flower structure. The opposite end of the stepover, near Cairo Sulcus is identified by a parallel system of narrow, sub-kilometer high ridges that curve ~90 that appear to form a (transpressional) restraining bend. Suggested axial discontinuities along the three visible tiger stripes in Fig. 1 each exhibit an apparent CCW rotational twist suggesting that they have all been deformed in response a left-lateral system of shear parallel to overall trend of the fractures and often mirrored by quasi-parallel, curvilinear patterns in the ropy plains between the tiger stripes. The presence of a distinct, 750m-high pair of narrow ridges centered on the Damascus discontinuity suggests that narrow dorsa within the tiger stripes (i.e. "shark fins") may be transpressional features, like those we've interpreted to form within restraining bends. This is also suggested by the morphological resemblance of stratigraphically old, degraded medial dorsa within sections of Baghdad Sulcus to positive flower structures [9,10]. References: [1] Nimmo, F. et al. (2007). Nature 447, 289-291; [2] Hurford, T. et al. [9] Helfenstein, P. et al. (2011). Tectonism and Terrain Evolution on Enceladus: I. Tectonic features and patterns (submitted); [10] Helfenstein, P. et al. (2011). Tectonism and Terrain Evolution on Enceladus: II. Interpretation and Hypotheses (submitted). FIGURE 1 (next page): Tectonic unit map (left) and corresponding 28m/pixel photomosaic (right) show tectonic patterns of the South Polar Terrain region. Proposed axial discontinuities along tiger stripes are shown by curved arrows labeled "A" (dashed arrows indicate least certain interpretation). From top to bottom are Damascus, Baghdad, and Cairo Sulci. Stepover extends from a releasing bend near Damascus Sulcus to a restraining bend at the corresponding end of Baghdad.
    2011 Enceladus Focus Group Meeting, SETI Institute, Mountain View, CA; 05/2011
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    ABSTRACT: The evolution of the spin rate of Comet 9P/Tempel 1 through two perihelion passages (in 2000 and 2005) is determined from 1922 Earth-based observations taken over a period of 13year as part of a World-Wide observing campaign and from 2888 observations taken over a period of 50 days from the Deep Impact spacecraft. We determine the following sidereal spin rates (periods): 209.023±0.025°/dy (41.335±0.005h) prior to the 2000 perihelion passage, 210.448±0.016°/dy (41.055±0.003h) for the interval between the 2000 and 2005 perihelion passages, 211.856±0.030°/dy (40.783±0.006h) from Deep Impact photometry just prior to the 2005 perihelion passage, and 211.625±0.012°/dy (40.827±0.002h) in the interval 2006–2010 following the 2005 perihelion passage. The period decreased by 16.8±0.3min during the 2000 passage and by 13.7±0.2min during the 2005 passage suggesting a secular decrease in the net torque. The change in spin rate is asymmetric with respect to perihelion with the maximum net torque being applied on approach to perihelion. The Deep Impact data alone show that the spin rate was increasing at a rate of 0.024±0.003°/dy/dy at JD2453530.60510 (i.e., 25.134 dy before impact), which provides independent confirmation of the change seen in the Earth-based observations.The rotational phase of the nucleus at times before and after each perihelion and at the Deep Impact encounter is estimated based on the Thomas et al. (Thomas et al. [2007]. Icarus 187, 4–15) pole and longitude system. The possibility of a 180° error in the rotational phase is assessed and found to be significant. Analytical and physical modeling of the behavior of the spin rate through of each perihelion is presented and used as a basis to predict the rotational state of the nucleus at the time of the nominal (i.e., prior to February 2010) Stardust-NExT encounter on 2011 February 14 at 20:42.We find that a net torque in the range of 0.3–2.5×107kgm2s−2 acts on the nucleus during perihelion passage. The spin rate initially slows down on approach to perihelion and then passes through a minimum. It then accelerates rapidly as it passes through perihelion eventually reaching a maximum post-perihelion. It then decreases to a stable value as the nucleus moves away from the Sun. We find that the pole direction is unlikely to precess by more than ∼1° per perihelion passage. The trend of the period with time and the fact that the modeled peak torque occurs before perihelion are in agreement with published accounts of trends in water production rate and suggests that widespread H2O out-gassing from the surface is largely responsible for the observed spin-up.
    Icarus 05/2011; 213:345-368. · 3.16 Impact Factor
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    ABSTRACT: Until November 2009 the relation of the tectonic styles on the leading hemisphere of Enceladus to those elsewhere on the satellite were unclear. Cassini's ISS Narrow Angle Camera (NAC) acquired high-resolution mosaics of the leading hemisphere for the first time during three close flybys, one on November 21, 2009, another on May 18, 2010, and a third on August 13, 2010, respectively. The new mosaics show that the leading side has distinct geological provinces that exhibit diverse tectonic styles and different cratering histories. The highly tectonised terrains are bounded by a prominent broad annulus of grooved and striated terrains that ranges from about 60 km to over 140 km in width. It surrounds a complex arrangement of tectonic structures, including a conspicuous province near 30°N, 90°W of curvilinear massifs and roughly orthogonal-trending ridged-troughs that define a crudely radial and concentric pattern relative to a point near 25°N, 125°W. This angular sector, about 65° in width, may be the partial remains of an ancient impact basin with a diameter of about 180 km. It could also be the surface expression of an ancient, large diapir. The peculiar quasi-radial ridged-troughs resemble extinct, topographically degraded examples of tiger stripes seen elsewhere on Enceladus. While these features may have a different fracture origin from tiger stripes, their comparable morphology suggests that long ago they may have expressed a similar style of fissure volcanism. Among our other significant findings is a region near 10°S, 60°W of rounded, rope-like sub-parallel ridges similar to ropy (funiscular) plains materials previously found only in the South Polar Terrain region near active tiger stripes. We suggest that the pattern of ropy ridges on the leading hemisphere arose from a similar style of tectonic deformation that produced the South Polar funiscular plains – a terrain that is closely related to possible folding and tectonic spreading associated with the tiger stripes. These features may thus record an ancient episode of South Polar style tectonism and volcanism near the equator. This hypothesis is consistent with the observed presence of viscously relaxed impact craters at the boundaries of the tectonically modified leading-side terrains as probes of a formerly elevated regional heat flux.
    AGU Fall Meeting; 12/2010
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    ABSTRACT: The Amor mission will rendezvous and land at the triple Near-Earth Asteroid system (153591) 2001 SN263 and execute detailed, in-situ science investigations. The spacecraft reaches 2001 SN263 by using a two-year DeltaVEGA (DeltaV-Earth Gravity Assist) trajectory with a relatively low launch C3 of 33.5 km2/s2. Rendezvous will enable reconnaissance activities including global and regional imaging, shape modeling, system dynamics, and compositional mapping. After landing, Amor will conduct in-situ imaging (panoramic to microscopic scale) and compositional measurements to include elemental abundance. The main objectives are to 1) establish in-situ the long-hypothesized link between C-type asteroids and the primitive carbonaceous chondrite (CC) meteorites, 2) investigate the nature, origin and evolution of C-type asteroids, and 3) investigate the origin and evolution of a multiple asteroid system. The mission also addresses the distribution of volatiles and organic materials, impact hazards, and resources for future exploration. Amor is managed by NASA Ames Research Center in partnership with Orbital Sciences, KinetX, MDA, and Draper with heritage instruments provided by Ball Aerospace, JHU/APL, and Firestar Engineering. The science team brings experience from NEAR, Hayabusa, Deep Impact, Dawn, LCROSS, Kepler, and Mars missions. In this paper, we describe the science, mission design, and main operational challenges of performing in-situ science at this triple asteroid system. Challenges include landing on the asteroid components, thermal environment, short day-night cycles, and the operation of deployed instruments in a low gravity (10^-5 g) environment.
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    ABSTRACT: The scientific goals of the Stardust-NExT mission to comet 9P/Tempel 1 include imaging 25% of the area imaged by the Deep Impact mission at a resolution of at least 80 m/pixel looking for changes to the surface, imaging, at the highest possible resolution, of the artificial crater created during the Deep Impact encounter (349W, -26), and imaging coverage of a portion of the terrain not yet seen. Fulfilling these goals required detailed knowledge of the spin state of 9P's nucleus approximately one year ahead of the nominal time of encounter, Feb 14, 2011. Since the encounter occurs 33 days after perihelion passage it was necessary to develop a model of the acceleration of the comet's spin state through perihelion passage in order to make a prediction. Determination of the spin state to the required accuracy was achieved in January, 2010, and was accomplished using observations taken from the Hubble Space Telescope and from ground-based observatories. This information was then used as the basis of trajectory correction maneuver in Feb, 2010. We describe the independent development of two spin rate acceleration models based on 13 years of observations of the rate and phase of spin of the comet's nucleus through two perihelion passages obtained with the Hubble and Spitzer Space Telescopes, many ground-based telescopes within the organization of a International World-Wide campaign (Meech et al., 2005), and the Deep Impact mission. We present a visualization of the encounter that shows the anticipated coverage of the surface of 9P/Tempel 1 that should be attained and emphasizes the proportion of the surface previously seen with the Deep Impact cameras and the new terrain that will be covered. Meech, K.J, and 210 coauthors. 2005. Deep Impact: Observations from a World-Wide Earth-based Campaign. Science 310, 265-269.

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8k Citations
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  • 1972–2013
    • Cornell University
      • • Center for Radiophysics and Space Research (CRSR)
      • • Department of Astronomy
      New York City, NY, United States
  • 2005–2010
    • Cornell College
      Cornell, Wisconsin, United States
    • The Space Science Institute
      Boulder, Colorado, United States
  • 2006
    • Freie Universität Berlin
      • Institute of Geological Sciences
      Berlin, Land Berlin, Germany
  • 2001
    • SAIC
      Belton, Texas, United States
  • 2000
    • Massachusetts Institute of Technology
      • Department of Earth Atmospheric and Planetary Sciences
      Cambridge, MA, United States
    • Johns Hopkins University
      • Applied Physics Laboratory
      Baltimore, MD, United States
  • 1998
    • United States Geological Survey
      Reston, Virginia, United States
    • The University of Arizona
      • Department of Planetary Sciences
      Tucson, AZ, United States
    • University of Toledo
      Toledo, Ohio, United States
  • 1974–1998
    • Stanford University
      Palo Alto, California, United States
  • 1997
    • Malin Space Science Systems
      San Diego, California, United States
  • 1976
    • Santa Clara University
      Santa Clara, California, United States
    • Harvard University
      Cambridge, Massachusetts, United States
  • 1969
    • Cambridge College
      Cambridge, Massachusetts, United States