NEAR-Shoemaker carried several instruments, but two are central to determining the mineralogical and chemical composition of the asteroid: the x-ray gamma-ray spectrometer (XGRS for short) and the NEAR infrared spectrometer (NIS). The only problem is that we do not know which asteroid each type of meteorite comes from, with one exception. The exception is a group of meteorites called howardites, eucrites, and diogenites (nicknamed HED meteorites). "The composition of 433 Eros: A mineralogical-chemical synthesis." The HED meteorites (howardites, eucrites, and diogenites) are basalt lava flows (eucrites), coarse-grained igneous rocks (diogenites), or mixtures of the two (howardites). View/ Open. For an asteroid of similar size to 433 Eros containing only 10% of its mass as a rare-precious metal like platinum, well that's when you get the capability to buy out the entire planet. Lodranites, which are the residues of partial melting, have very low sulfur/silicon ratios. As mixtures of iron, nickel, and sulfur are heated, the first melt to form is very rich in sulfur, containing about 30 wt%. We report major element composition ratios for regions of the asteroid 433 Eros imaged during two solar flares and quiet sun conditions during the period of May to July 2000. Too bad it is not easy to do. The consensus was that they are mixtures of iron-magnesium silicates with some metallic iron, but that is where the agreement ended. of Space & Aeronaut-ical Sci., 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan. Beth Clark concludes that the spectral variations might be caused by an enhanced concentration of iron sulfide (the mineral troilite), which darkens the material, combined with lunar-like space weathering. We do not know much about space weathering on asteroids. The spectra of reflected light cannot be interpreted in any straightforward way. The instrument payload is in the golden area beneath the blue solar panels. In March 2000 the spacecraft was named after Eugene Shoemaker, a brilliant, insightful planetary geologist and great man. One group of asteroids, the S-asteroids, has been the subject of spirited debate during the past two decades. It is the most well studied asteroid. Derek Sears (University of Arkansas) and a group of colleagues are developing a concept for an asteroid sample-return mission. These scientific data -- the first ever collected on the surface of an asteroid -- result from 7 days of measurements following NEAR Shoemaker's historic landing on February 12. The way light reflects depends on the grain sizes of the minerals, the temperature, the sun angle, and the extent of space weathering, besides what minerals are present. Eros, 33 x 13 x 13 kilometers, looks like a giant peanut. If you wish to distribute this article to others, you can order high-quality copies for your € following the guidelines here. Scientists suspect that its angular shape resulted from violent impacts. These results facilitated the use of the gamma-ray measurements to produce the first in situ measurement of hydrogen concentrations on an asteroid. Gamma-Ray Readings from Eros This chart shows the gamma-ray spectrum from the surface of Eros. Artist's conception of the NEAR-Shoemaker spacecraft in space. Instead, we ended up with a plethora of tiny planets. Chondrites are similar at wavelengths less than 1.5 microns, but differ at longer wavelengths. Courtesy Applied Physics Laboratory. Some S-asteroids have spectra similar to some partially melted meteorite groups, but not all do. 433 Eros live position and data. The measured value, 1100-700+1600 ppm, … Eros is 20 miles (33 kilometers) long and about 8 miles (13 kilometers) wide. Instead, the NEAR team used ratios of elements. The spacecraft would obtain samples from several places on three different asteroids and return them to Earth. It was able to measure rectangular regions on the surface of about 650 x 1300 meters, or square regions 1300 x 1300 meters. It is all quite tricky (and explains why I work with other types of data). He also established the lunar geological time scale, which allowed us to date the relative ages of features on the Moon. Venn diagrams, which examine overlapping features in two data sets, suggest that the best match for 433 Eros is an ordinary chondrite, altered at the surface of the asteroid, or perhaps a primitive achondrite derived from material mineralogically similar to these chondrites. The NIS was a spectrograph that used a diffraction grating to disperse the infrared light reflected from the asteroid onto two electronic detector arrays. They are also a natural laboratory for studying what happens when small bodies melted, sometimes forming cores and mantles like the Earth. © 2016 The Author. NEAR Science Results from Asteroid 433 Eros. No type fits exactly, though some candidates are clearly better than others. Psyche crater (5.3 kilometers in diameter) dominates one hemisphere of Eros (left). Both give elemental abundances, but during the mission the gamma ray spectrometer had some difficulties and did not return useful data from orbit. Search DSpace This Collection. Written by G. Jeffrey TaylorHawai'i Institute of Geophysics and Planetology. Several factors affect the spectra of reflected light: the sizes of the grains making up the surface, the amounts of olivine and pyroxene (iron-magnesium silicates), and the effects of space weathering. High-resolution surface images and measurements made by NEAR's Laser Rangefinder have been combined into the above visualization based on the derived 3D model of the tumbling space rock. We report major element composition ratios for regions of the asteroid 433 Eros imaged during two solar flares and quiet sun conditions during the period of May to July 2000. Tim McCoy (Smithsonian Institution) and others synthesized all the observations to derive the best guess as to what type of meteorite is most similar to Eros. It stands for Near-Earth Asteroid Rendezvous. NEAR obtained new information on the nature and evolution of asteroids, improved our understanding of planetary … THE GLOBAL ELEMENTAL COMPOSITION OF 433 EROS: FIRST RESULTS FROM THE NEAR GAMMA-RAY SPECTROMETER ORBITAL DATASET. Primitive achondrites such as acapulcoites do not fit as well even at wavelengths shorter than 1.5 microns. Show full item record. This paper reviews the scientific results of THE NEAR MISSION. So, we have a dilemma: Two schools of thought arguing over ambiguous data. suggest that the best match for 433 Eros is an ordinary chondrite, altered at the surface of the asteroid, or perhaps a primitive achondrite derived from material mineralogically similar to these chondrites. Lessons for future gamma-ray spectrometer investigations are discussed. The Eros data are compared to LL ordinary chondrites and a primitive type of achondrite called acapulcoites. The NEAR science team did excellent, creative work in trying to determine which, if any, type of meteorite matches the properties of Eros. The x-ray spectrometer returned the abundances of magnesium, aluminum, silicon, iron, calcium, and sulfur. This dataset, which amounts to just ~10 h of data collection, was used to produce the first GRS-derived global elemental composition values. The data confirm prior conclusions that the elemental composition of Eros' surface is inconsistent with achondritic and volatile-rich carbonaceous chondritic compositions. At 40 X 14 X 14 km, it is the largest asteroid that approaches close to Earth. Low aluminum abundances for all regions argue against global differentiation of Eros. Asteroids give us clues to the nature of the planetesimals that accumulated to form the planets. Nittler argues that it might not be easy to lose the sulfur-rich melt without melting the silicate, too. Although most chemical parameters provide good fits between ordinary chondrites and Eros, the x-ray spectrometer measurements indicate that sulfur is much lower than in ordinary chondrites. Ida is a big sister look-alike to Gaspra, measuring 55 kilometers long. These work just as well for most purposes. Asteroids are planets whose growth was stunted when the solar system formed. Using measurements of x-rays emitted from the asteroid and light reflected off it, the consensus is that Eros is more like an ordinary chondrite than any other type, though a little bit of melting cannot be ruled out. Mathilde, 59x47 kilometers, is also decorated with countless craters, some of which are very large. The Dawn mission will orbit Vesta for a year, gathering photogeological, mineralogical, and chemical data, then move on to the largest asteroid 1 Ceres. Nevertheless, they do show that the possibilities are reasonably narrow. ESTIMATING THE COMPOSITION AND THE DEGREE OF SPACE WEATHERING OF ASTEROIDS 6 HEBE, 433 EROS, AND 25143 ITOKAWA BY REFLECTANCE SPECTROSCOPY USING A NEW MODELING APPROACH. Clark and co-workers scaled the reflectance to be exactly 1 at 1.4 microns so the shapes of the spectra could be compared easily. However, calculations by my colleagues Lionel Wilson and Klaus Keil show that sulfur-rich melts might be driven to the surface so fast that they would escape an asteroid. Unfortunately, they conclude that a unique solution is not possible. A reanalysis of NEAR X-ray/gamma-ray spectrometer (XGRS) data provides robust evidence that the elemental composition of the near-Earth asteroid 433 Eros is consistent with the L and LL ordinary chondrites. Magnesium/silicon, aluminum/silicon, calcium/silicon, and iron/silicon ratios are best interpreted as a relatively primitive, chondritic composition… What we need is chemical compositions of the surface materials and new ways of determining the identities and abundances of the minerals present on the surface. NEAR-Shoemaker mapped Eros in detail back in 2000-2001 before officials executed a controlled and dramatic crash landing, the first-ever touchdown on an asteroid. Their compositions, especially their high Mg/Si, rule them out as candidates for Eros. Explanation: Orbiting the Sun between Mars and Earth, asteroid 433 Eros was visited by the robot spacecraft NEAR-Shoemaker in 2000 February. Low aluminum abundances for all regions argue against global differentiation of Eros. The celestial coordinates, magnitude, distances and speed are updated in real time and are computed using high quality data sets provided by the JPL Horizons ephemeris service (see acknowledgements for details). Peeking inside the crater (right) we see lighter and darker regions formed when materials moved down the steep slopes. In fact, it is almost impossible to obtain reliable estimates of elemental abundances. The compositions of enstatite (E) chondrites and two types of carbonaceous chondrites (CV and CO) are not as consistent and can probably be ruled out. S-asteroids are a somewhat diverse group of little planets with similar characteristics in the spectra of light reflected from them. The best bet is that space weathering has affected the surface materials and altered the spectral properties. The primary goal of the mission was to study the near-Earth asteroid 433 Eros from orbit for approximately one year. Such a mission would also carry remote sensing instruments to help select sampling sites. The high-gain antenna above the solar cells is 1.5 meters across and was used to send data back to NASA's deep space network on Earth. Boulders and ponds on the Asteroid 433 Eros Andrew J. Dombarda,*, Olivier S. Barnouina, Louise M. Procktera, Peter C. Thomasb a The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., Laurel, MD 20723, United States bCenter for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, United States a r t i c l e i n f o This might be due to space weathering effects involving the volatilization of sulfur, or partial melting that removed sulfur-rich melts from the body. This probably happened because of the rapid assembly of Jupiter, the largest planet. Eros … Additional data restricts the match to L and LL chondrites. All of DSpace. Certainly not--we can always appeal to space weathering. 433 Eros, which have high albedos and reddish color. However, we have no primitive extraterrestrial material that contains so little sulfur. A primary goal of the Near-Earth Asteroid Rendezvous (NEAR) mission was to compare the elemental composition of the S-type asteroid 433 Eros to the chemical compositions of meteorites, with the specific objective of testing the hypothesis that the S-type asteroids are the source of the ordinary chondrite (OC) meteorites. Lucy McFadden (University of Maryland) and co-authors made a detailed study of the spectra taken of Eros and conclude that the spectral properties are consistent with that of an ordinary chondrite. The instrument recorded the intensity of light reflected at 64 different wavelengths between 804 and 2732 nanometers. This would seem to be contradictory to the XGRS data, which indicate that sulfur is depleted on the surface of Eros. Understanding it better was a goal of the NEAR mission. Magnesium/silicon, aluminum/silicon, calcium/silicon, and iron/silicon ratios are best interpreted as a relatively primitive, chondritic composition… Using a Venn diagram, they infer that only ordinary chondrites (if space weathered) and primitive achondrites match both the XGRS chemical data and the MSI, NIS mineralogical data. The optical differences imply differences in composition and origin, and within these general groups, many other subgroups have been suggested to organize possible compositional and miner- alogical differences. Composite spectra of different rotational aspects of the S asteroid 433 Eros were assembled from previous studies, covering the wavelength range 0ø33-2.5 grn. One measurement surprised the NEAR team. All the other types of meteorites come from somewhere out there, but we do not know where. As McCoy and his colleagues note, the way to get the highest fidelity information is to return samples from asteroids to Earth for intense study in laboratories. This item appears in the following Collection(s) Search DSpace. Normalized element distributions preclude FeO-rich … Clark's modeling calculations indicate that the spectral variations in Psyche cannot be caused solely by variations in grain size, olivine, pyroxene, or a moon-like weathering process. Nittler (Carnegie Institution of Washington) and others calculate that the upper 5 cm of Eros could have lost all its sulfur in 10 million years. Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology The Near-Earth Asteroid Rendezvous (NEAR) mission spent about a year orbiting the asteroid 433 Eros, a 33 x 13 x 13 km chunk of rock. The global elemental composition of 433 Eros: First results from the NEAR gamma-ray spectrometer orbital dataset. Charlois at Nice, France. Meteorites that formed by melting on their parent asteroids do not match the composition determined for Eros. Note the boulders (several meters across) collected in the bottom of the crater. The Spacers are zealous about non-composition – the band room is viscous, chasing the goal of free-improvisation within the realm of tempo based contemporary music. Witt's discovery was the accidental byproduct of a two-hour photographic exposure he conducted of a different asteroid: 185 Eunike. In principle, this allows us to identify which minerals are present, a key aid to rock identification. This is what one would expect from an unmelted asteroid or from one melted only very slightly. Chondrites were not melted after their components accreted to form asteroids and, thus, contain a wealth of information about the gas cloud surrounding the primitive Sun. If it is not just a surface effect, and the entire body is depleted in sulfur, perhaps it simply formed that way. A milestone in the study of asteroids occurred on 14 Feb 2000, when the NEAR spacecraft entered orbit around the asteroid 433 Eros for a year of detailed observation of the geology, mineralogy and chemistry of the surface, before landing on the surface on 12 Feb 2001 and conducting the first science on the surface of a small Solar System body. However, it takes only a few percent of a dark mineral to affect the brightness of a surface deposit. The sulfur/silicon ratio is far below that of ordinary chondrites (see diagram below). These effects can be modeled mathematically. It has an eight-position filter wheel covering the spectral range from 450 to 1100 nm (visible to near infrared). 433 Eros is a member of the "S" class of asteroids, which are composed of iron-containing silicates and metal. To date, no Eros-originating signal had been reported in GRS orbital measurements, a consequence of NEAR's high orbital altitudes about Eros. More asteroids need to be visited and samples returned from them. This page shows Asteroid 433 Eros location and other relevant astronomical data in real time. This turns out to be a lucky thing because asteroids preserve a record of the processes that operated as the solar system was forming from a cloud of gas and dust. Copyright © 2021 Elsevier B.V. or its licensors or contributors. Ureilites are complicated carbon-bearing rocks that appear to be the residues from partial melting of an asteroid. Normalized element distributions preclude FeO-rich pyroxenes and suggest that the x-ray and gamma- Other factors must be operating. (433) Eros ist ein Asteroid, der am 13. One school of thought identified them as related to ordinary chondrites, the most common type of meteorite observed to fall on Earth. Alternatively, the sulfur might have been lost through partial melting. This explanation is unlikely. 433 Eros Scott L. Murchie Applied Physics Laboratory, The Johns Hopkins University, Laurel, Maryland Carle M. Pieters Department of Geological Sciences, Brown University, Providence• Rhode Island Abstract. Even in the low gravity of a small asteroid, rock and dirt can slide downhill, leaving behind patches of fresher, lighter materials. Most minerals reflect visible and infrared light in unique ways. They are very different in composition from Eros. T. Nimura1, M. Abe1, T. Hiroi2 and C. M. Pieters2, 1JAXA Inst. It might be a piece of a larger asteroid that was blown apart by a giant impact. This is a plot of the relative amount of light reflected in wavelengths from 0.8 to 2.5 microns on Eros. When placed in the context of other gamma-ray spectrometer investigations, this analysis indicates that successful gamma-ray spectroscopy investigations require extended periods of time (≥10 days) at orbital altitudes less than or equal to the radius of the target body. Data from the x-ray spectrometer consists of counts of x-rays with different energies. This measurement of one S-asteroid, however, has not settled the argument. Results include the first absolute concentrations of Fe and Th, and the first global K concentration. NH-Mineral Sciences. Cynics might say that there is nothing like a mysterious process to help save your idea from the harsh reality of data, but we know from studies of the Moon that the spectral properties of planetary materials are changed by exposure to solar wind and micrometeorite impacts. The HED meteorites apparently come from asteroid 4 Vesta. We need more precise mineralogical and chemical data of both surface materials and bedrock. It takes a heroic effort to convert these to percentages of elements (see article by Nittler and others). In the Venn diagram, the types of meteorites outside any circle do not have chemical or spectral properties like those of Eros. 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