Japan Geoscience Union Meeting 2019

Presentation information

[E] Oral

P (Space and Planetary Sciences ) » P-PS Planetary Sciences

[P-PS03] Solar System Small Bodies: A New Frontier Arising Hayabusa 2, OSIRIS-REx and Other Projects

Wed. May 29, 2019 9:00 AM - 10:30 AM A01 (TOKYO BAY MAKUHARI HALL)

convener:Masateru Ishiguro(Department of Physics and Astronomy, Seoul National University), Taishi Nakamoto(Tokyo Institute of Technology), Masanao Abe(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency), Olivier S Barnouin(Johns Hopkins University Applied Physics Laboratory), Chairperson:Taishi Nakamoto(Tokyo Institute of Technology)

9:15 AM - 9:30 AM

[PPS03-20] Global Geology of Bennu from NASA's OSIRIS-REx Space Mission

★Invited Papers

*Erica R Jawin1, Kevin J Walsh2, Tim McCoy1, Harold C Connolly3, Dante S Lauretta4, Ron L Ballouz4, Olivier S Barnouin5, C Beddingfield6, Carina A Bennett4, Edward B Bierhaus7, Keara N Burke4, Ben Clark8, Michael G Daly9, Marco Delbo10, Daniella DellaGiustina4, Jason P Dworkin11, Christine Hartzell12, John Marshall6, Patrick Michel10, Jamie L. Molaro13, Mike Nolan4, Maurizio Pajola14, Mark Perry5, Bashar Rizk4, Scott Sandford15, Dan J Scheeres16, Stephen R Schwartz4, David Trang17 (1.Smithsonian National Institute, Washington, DC, USA, 2.Southwest Research Institute, Boulder, CO, USA, 3.Dept. of Geology, Rowan University, Glassboro, NJ, USA, 4.Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA , 5.The Applied Physics Laboratory, Johns Hopkins University, Laurel, MD, USA, 6.SETI Institute, Mountain View, CA, USA, 7.Lockheed Martin Space Systems Company, USA, 8.Space Science Institute, Boulder CO, USA, 9.York University, Canada, 10.Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France, 11.NASA Goddard Space Flight Center, Greenbelt, MD, USA, 12.Department of Aerospace Engineering, University of Maryland, College Park MD, USA, 13.Planetary Science Institute, Tucson, AZ, USA, 14.INAF - Astronomical Observatory of Padova, Italy, 15.NASA Ames Research Center, USA, 16.Dept. of Aerospace Engineering Sciences, University of Colorado, Boulder, CO, USA, 17.HIGP/University of Hawaii at Manoa, USA)

Keywords:OSIRIS-REx, Bennu, Asteroid, Geology

NASA’s OSIRIS-REx sample return mission has been observing the near-Earth Asteroid (101955) Bennu since December 2018 and will be collecting a sample of the surface in the summer of 2020, to be returned to Earth in 2023. Preliminary and ongoing observations have yielded much information about Bennu’s formation, evolution, and ongoing geologic activity. Here we report on the global geology of Bennu based on analyses of images combined with shape, mass, and slope measurements. Initial results suggest that Bennu is a rubble-pile asteroid, formed from a parent body that was collisionally disrupted and reaccumulated. The asteroid has a “top” shape which is spherical with an equatorial bulge, similar to other near-Earth asteroids including Ryugu as observed by the Hayabusa2 sample return space mission. Candidate impact craters have been observed at a range of diameters between ~10-150 m across the surface of Bennu, leading to a crater retention age of 100 million to 1 billion years. An apparent concentration of large crater candidates at low latitudes suggest that the equatorial ridge is stratigraphically old, and may have formed early in Bennu’s history or been inherited from the reaccumulation event which created the asteroid. Several linear features have been identified on Bennu, the largest of which are topographic highs that extend longitudinally from the northern polar regions to the equator. Boulders are concentrated between several of these linear ridges, as well as in the interior of large candidate craters. Boulders on Bennu appear to be geologically diverse. Boulder sizes range from < 3 m to ~95 m in diameter with large variations in geometric albedo, morphology, degree of burial, and state of degradation. Fractured boulders have been identified with various numbers, orientations, and widths of fractures. Distinct clasts within several boulders indicate they may be breccias, while piles of boulders may represent disaggregated polymict or brecciated boulders. Current imaging resolution cannot resolve centimeter-sized particles, so direct detections of regolith or other sub-cm sized particles have not been made. However, several small candidate craters (< 20 m diameter) have a significant lack of boulders relative to the surrounding terrain, and additional datasets suggest the presence of a component of fine-grained particles. Improved image resolution will aid in the identification of regolith deposits on Bennu.