Variations in color and reflectance on the surface of asteroid (101955) Bennu
The complex history of Bennu's surface
The near-Earth asteroid (101955) Bennu is a carbon-rich body with a rubble pile structure, formed from debris ejected by an impact on a larger parent asteroid. The Origins, Spectral Interpretation, Resource Identification, Security, Regolith Explorer (OSIRIS-REx) spacecraft is designed to collect a sample of Bennu's surface and return it to Earth. After arriving at Bennu, OSIRIS-REx performed a detailed survey of the asteroid and reconnaissance of potential sites for sample collection. Three papers present results from those mission phases. DellaGiustina et al. mapped the optical color and albedo of Bennu's surface and established how they relate to boulders and impact craters, finding complex evolution caused by space weathering processes. Simon et al. analyzed near-infrared spectra, finding evidence for organic and carbonate materials that are widely distributed across the surface but are most concentrated on individual boulders. Kaplan et al. examined more detailed data collected on the primary sample site, called Nightingale. They identified bright veins with a distinct infrared spectrum in some boulders, which they interpreted as being carbonates formed by aqueous alteration on the parent asteroid. Together, these results constrain Bennu's evolution and provide context for the sample collected in October 2020.
Structured Abstract
INTRODUCTION
The color and reflectance of asteroids can be used to infer their compositions and histories. Variations in these spectrophotometric properties are driven by differences in lithology and/or exposure to processes collectively known as space weathering (bombardment by meteoroids and solar wind ions). On anhydrous bodies, such as the Moon and S-type asteroids, space weathering darkens and reddens spectral slopes (where “redder” indicates a more positive slope relative to the solar spectrum) in the visible wavelengths. However, on primitive C-complex asteroids—bodies that may have delivered water and organics to early Earth—the spectral changes that result from space weathering are not well understood. Evidence from meteorites thought to be analogous to C-complex asteroids suggests that either reddening or bluing is possible. Deciphering such changes is necessary to understand the origin and relative exposure age of surface units on primitive Solar System objects.
RATIONALE
The MapCam imager on the OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer) spacecraft acquired global multispectral images of the C-complex asteroid (101955) Bennu in four bands: b′ (0.44 to 0.50 μm), v (0.52 to 0.58 μm), w (0.67 to 0.73 μm), and x (0.82 to 0.89 μm). Bennu is a rubble pile, made up of the reaccumulated fragments of a larger C-complex progenitor that was blown apart by a catastrophic impact.
Using band ratios and principal components analysis, we mapped Bennu’s color and reflectance at a pixel scale of ~25 cm. In combination with higher-resolution (~5 cm per pixel) panchromatic PolyCam images, we assessed relationships between MapCam spectra and morphologic features on Bennu’s surface, aiming to understand sources of variation from the average and determine the relative timing associated with color differences.
RESULTS
The surface of Bennu has unexpectedly heterogeneous colors distributed on a moderately blue (gently negatively sloped) global surface. Boulders are the dominant source of heterogeneity and fall into distinct populations on the basis of reflectance. Dark boulders (reflectance of 0.034 to 0.049, encompassing Bennu’s average reflectance of 0.044) tend to be rougher and rounder, whereas bright boulders (0.049 to 0.074) are smoother and more angular. Variation in color within individual boulders is also apparent; for example, boulder faces that appear to be more recently exposed owing to fracturing are bluer than putatively older faces. Conversely, small reddish craters are observed to overlie blue craters, indicating that the former are younger (more recently exposed material). Bennu’s smallest craters have a size distribution that indicates that they are also the youngest, and they are redder than the average surface. Many of the larger (older) craters have colors indistinguishable from Bennu’s average. Crater spectral slopes indicate that terrains with intermediate ages have the bluest near-ultraviolet spectral slopes.
CONCLUSION
The differences in reflectance and texture among boulders indicate that Bennu may have inherited distinct lithologies formed at different depths in its larger progenitor asteroid, as well as debris from impactors. The color variations within boulders and among craters suggest that space weathering on Bennu does not drive a unidirectional progression from red to blue (or vice versa). Rather, freshly exposed redder surfaces, as exemplified by the small reddish craters, initially brighten in the near-ultraviolet region (i.e., become blue at shorter wavelengths), as exemplified by blue crater rims and fractured boulder faces. Brightening in the visible to near-infrared wavelengths follows, ultimately leading to more moderately blue spectral slopes, consistent with Bennu’s average. The time scale associated with space weathering–induced color changes (~105 years) is compatible with previous findings only if Bennu’s small reddish craters formed under conditions in which gravity, rather than the strength of the impacted surface, is the dominant influence. This finding offers an indication of cratering physics on small rubble-pile asteroids.
False-color image mosaic of rubble on asteroid Bennu, as observed with the MapCam multispectral imager.
Color and reflectance vary between and within boulders, resulting from different exposure ages and innate compositions. Red is the x/v band ratio (indicating redder spectral slopes), green represents relative change in the w band (an indication of composition), and blue is the b′/v band ratio (indicating bluer spectral slopes in the near-ultraviolet region).
Abstract
Visible-wavelength color and reflectance provide information about the geologic history of planetary surfaces. Here we present multispectral images (0.44 to 0.89 micrometers) of near-Earth asteroid (101955) Bennu. The surface has variable colors overlain on a moderately blue global terrain. Two primary boulder types are distinguishable by their reflectance and texture. Space weathering of Bennu surface materials does not simply progress from red to blue (or vice versa). Instead, freshly exposed, redder surfaces initially brighten in the near-ultraviolet region (i.e., become bluer at shorter wavelengths), then brighten in the visible to near-infrared region, leading to Bennu’s moderately blue average color. Craters indicate that the time scale of these color changes is ~105 years. We attribute the reflectance and color variation to a combination of primordial heterogeneity and varying exposure ages.
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Supplementary Material
Summary
Materials and Methods
Figs. S1 to S16
Tables S1 and S2
Data S1 to S3
Resources
References and Notes
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Acknowledgments
We thank the entire OSIRIS-REx Team for making the encounter with Bennu possible. For fig. S5, we thank D. Rachford and IMV Minerals for providing the SAP105 sample and S. Mertzman of Franklin and Marshall College for confirming the composition of the SAP105 sample. We thank R. J. Burmeister for assistance with graphic design of the figures. Funding: D.N.D., K.N.B., K.J.W., P.H.S., D.R.G., E.B.B., R.L.B., T.B., H.C., B.E.C., A.S., K.B., C.A.B., W.F.B., J.I.B., H.C.C., C.Y.D.D., K.L.E., V.E.H., C.W.H., E.S.H., E.R.J., H.H.K., L.L.C., L.L., J.Y.L., M.C.N., J.N., N.A.P., B.Ri., A.J.R., N.K.S., A.A.S., C.W.V.W., and D.S.L. were supported by NASA under contract NNM10AA11C issued through the New Frontiers Program. J.L.M. and D.T. were supported by the NASA OSIRIS-REx Participating Scientist Program 80NSCC18K0230. A.R.H. was supported by the NASA Solar System Exploration Research Virtual Institute 2016 (SSERVI16) Cooperative Agreement TREX NNH16ZDA001N. E.T., K.Y., and S.S. were supported by the Japanese Society for Promotion of Science (JSPS) Core-to-Core program “International Planetary Network.” The OLA instrument and funding for M.G.D. and M.M.A.A. and support for A.P., E.A.C., and D.M.A., were provided by the Canadian Space Agency. J.L.R., E.T., M.Po., and J.d.L. acknowledge support from the project AYA2017-89090-P of the Spanish MINECO and from the project ProID2017010112 under the OP-ERDF-ESF and the Canarian Agency for Research, Innovation and Information Society (ACIISI). M.Pa. was supported by the Italian Space Agency (ASI) under the ASI-INAF agreement no. 2017-37-H.0. C.A., J.D.P.D., M.A.B., M.D., P.H.H., P.M., and S.F. acknowledge support from the French space agency CNES. P.M. also acknowledges support from the European Union’s Horizon 2020 research and innovation program under grant agreement no. 870377 (project NEO-MAPP). C.A. was also supported by the French National Research Agency under the project “Investissements d’Avenir” UCAJEDI (ANR-15-IDEX-01). C.A. and M.D. also acknowledge support from the ANR “ORIGINS” (ANR-18-CE31-0014). B.Ro. acknowledges support from the Royal Astronomical Society (RAS) and the UK Science and Technology Facilities Council (STFC). Author contributions: D.N.D., P.H.S., D.R.G., B.Ri., and C.Y.D.D. planned and calibrated OCAMS MapCam and PolyCam observations of Bennu. D.N.D., K.N.B., P.H.S., D.R.G., T.L.B., K.J.B., C.A.B., J.I.B., K.L.E., L.L.C., and N.K.S. created MapCam color parameter maps of Bennu. K.N.B., E.B.B., J.N., D.T., and R.B.V.A. mapped craters and boulders on Bennu. D.N.D., K.N.B., K.J.W., P.H.S., E.B.B., R.-L.B., M.M.A.A., and W.F.B. performed the statistical analysis of boulder and craters colors. E.T., K.Y., and S.S. performed comparisons of the colors of Bennu and Ryugu. E.A.C., B.E.C., A.R.H., A.S., D.M.A., and A.P. performed comparisons between Bennu colors and laboratory spectra. J.D.P.D., A.A.S., H.H.K., and V.E.H. processed and interpreted OVIRS observations of Bennu. M.G.D., M.M.A.A., R.-L.B., and N.A.P. processed and interpreted OLA observations of Bennu. D.N.D., P.H.S., D.R.G., K.J.W., R.-L.B., H.C., C.A., M.A.B., H.C.C.Jr., M.D., J.d.L., S.F., V.E.H., P.H.H., C.W.H., E.S.H., E.R.J., H.H.K., L.F.L., J.Y.L., P.M., J.L.M., M.C.N., M.Pa., M.Po., A.J.R., B.Ro., A.A.S., D.T., and C.W.V.W. contributed to the conceptualization and writing. D.S.L. contributed to the conceptualization and leads the OSIRIS-REx mission. Competing interests: We declare no competing interests. Data and materials availability: Full-resolution MapCam color maps of Bennu, as shown in Fig. 1 and fig. S5, are available at figshare (72). Catalogs of the boulders and craters we used are available as data S1 and S2, respectively. The stereophotoclinometry v28 and OLA v20 shape models of Bennu are available through the Small Body Mapping Tool at http://sbmt.jhuapl.edu/. Detailed Survey OCAMS (MapCam and PolyCam), Orbital B OLA, and Detailed Survey and Recon A OVIRS data are available via the Planetary Data System (PDS) at: https://sbnarchive.psi.edu/pds4/orex/orex.ocams/data_calibrated/detailed_survey/, https://sbnarchive.psi.edu/pds4/orex/orex.ocams/data_calibrated/recon/, https://sbnarchive.psi.edu/pds4/orex/orex.ola/data_calibrated/orbit_b/, https://sbnarchive.psi.edu/pds4/orex/orex.ovirs/data_calibrated/detailed_survey/, and https://sbnarchive.psi.edu/pds4/orex/certified/orex.ovirs/data_calibrated/recon/, respectively. The list of MapCam images used to produce the maps in Fig. 1 is available as data S3.
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- The astrophysical context of collision processes in meteorites, Meteoritics & Planetary Science, 56, 7, (1406-1421), (2021).https://doi.org/10.1111/maps.13716
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