The dynamic geophysical environment of (101955) Bennu based on OSIRIS-REx measurements

Highsmith, D. E.; Small, Jeffrey L.; Vokrouhlický, David; Bowles, N. E.; Brown, Eloïse; Hanna, K. L. Donaldson; Warren, T.; Brunet, Claude; Chicoine, R. A.; Desjardins, Serge; Gaudreau, D.; Haltigin, T.; Millington-Veloza, S.; Rubi, A.; Aponte, José C.; Gorius, N.; Lunsford, Allen; Allen, B.; Grindlay, Jonathan E.; Guevel, D.; Hoak, D.; Hong, Jaesub; Schrader, D. L.; Bayron, J.; Golubov, Oleksiy; Sánchez, Paul; Stromberg, J.; Hirabayashi, Masatoshi; Hartzell, C. M.; Oliver, S.; Rascon, M.; Harch, A.; Joseph, J.; Squyres, S. W.; Richardson, D. C.; Emery, Joshua P.; McGraw, L.; Ghent, R. R.; Binzel, Richard P.; Asad, M. Al; Johnson, C. L.; Philpott, L.; Susorney, H. C. M.; Cloutis, E. A.; Hanna, R. D.; Connolly, H. C.; Ciceri, F.; Hildebrand, A. R.; Ibrahim, E.-M.; Breitenfeld, L. B.; Glotch, T. D.; Rogers, A. D.; Clark, B. E.; Ferrone, Salvatore; Thomas, C. A.; Campins, H.; Fernández, Yanga; Chang, Wen‐Yen; Cheuvront, A.; Trang, D.; Tachibana, Shogo; Yurimoto, Hisayoshi; Brucato, J. 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J.; Becker, T. L.; Bendall, S. P.; Bennett, C. A.; Bloomenthal, H.; Blum, Daniel; Boynton, W. V.; Brodbeck, J.; Burke, K. N.; Chojnacki, M.; Colpo, A.; Contreras, J. L.; Cutts, J. A.; d’Aubigny, C. Drouet; Dean, David A.; DellaGiustina, D. N.; Diallo, B.; Drinnon, D.; Drozd, Kristofer; Enos, H.; Enos, R.; Fellows, C.; Ferro, T.; Fisher, Matthew R.; Fitzgibbon, G.; Fitzgibbon, Mike; Forelli, J.; Forrester, T.; Galinsky, I.; García, R.; Gardner, Andrew; Golish, D. R.; Habib, Namrah; Hamara, D.; Hammond, D.; Hanley, Kevin J.; Harshman, K.; Hergenrother, C. W.; Herzog, Katja; Hill, D. H.; Hoekenga, C.; Hooven, S.; Howell, E. S.; Huettner, E.; Janakus, A.; Jones, J. Bryan; Kareta, Theodore; Kidd, John; Kingsbury, K.; Balram‐Knutson, S. S.; Koelbel, L.; Kreiner, J. M.; Lambert, Diane; Лауретта, Д. 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B.; Roberts, J. H.; Steele, R.; Turner, Rhiannon; Backer, J.; Edmundson, K. L.; Mapel, J.; Milazzo, M. P.; Sides, S.; Manzoni, C.; May, Brian Harold; Delbò, M.; Libourel, G.; Michel, Patrick; Ryan, A. J.; Thuillet, Florian; Marty, Bernard

doi:10.1038/s41550-019-0721-3

Cited by 140 publications

(161 citation statements)

References 35 publications

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“…With these objectives in mind, we carefully planned a large number of thermal observations during the ~1.5 years of proximity operations before sampling the surface. The Approach-phase observations described here enable direct comparisons to previous Spitzer Space Telescope observations of Bennu and provide the first direct test of the Yarkovsky effect [23]. Data from the Preliminary Survey mission phase in December 2018 provided the first disk-resolved thermal data of Bennu.…”

Section: Supplementary Materialsmentioning

confidence: 76%

“…This suggests that while the absolute number of large boulders on rubble-pile NEAs is scaled by asteroid size, surface particle distributions may be distinct on top-shaped objects. Notably, the distribution of the large boulders (≥20 m) at high latitudes on Bennu corresponds with a steepening in the dynamic surface slope outside of the equatorial latitudes [23]. Accordingly, material from midlatitude to polar regions is less energetically coupled to the surface of the asteroid [23].…”

Section: Spatially Resolved Surface Morphology and Boulder Distributionmentioning

confidence: 97%

“…Notably, the distribution of the large boulders (≥20 m) at high latitudes on Bennu corresponds with a steepening in the dynamic surface slope outside of the equatorial latitudes [23]. Accordingly, material from midlatitude to polar regions is less energetically coupled to the surface of the asteroid [23]. As a result, smaller particles may preferentially migrate away from these areas, resulting in the exhumation and retention of larger boulders at higher latitudes.…”

Section: Spatially Resolved Surface Morphology and Boulder Distributionmentioning

confidence: 98%

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Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis

et al. 2019

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Christensen, P. R.; Drouet d'Aubigny, C. Y.; Hamilton, V. E.; Reuter, D. C.; Rizk, B.; Simon, A. A.; Asphaug, E.; Bandfield, J. L.; Barnouin, O. S.; Barucci, M. A.; Bierhaus, E. B.; Binzel, R. P.; Bottke, W. F.; Bowles, N. E.; Campins, H.; Clark, B. C.; Clark, B. E.; Connolly, H. C.; Daly, M. G.; Leon, J. de; Delbo', M.; Deshapriya, J. D. P.; Elder, C. M.; Fornasier, S.; Hergenrother, C. W.; Howell, E. S.; Jawin, E. R.; Kaplan, H. H.; Kareta, T. R.; Le Corre, L.; Li, J.-Y.; Licandro, J.; Lim, L. F.; Michel, P.; Molaro, J.; Nolan, M. C.; Pajola, M.; Popescu, M.; Garcia, J. L. Rizos; Ryan, A.; Schwartz, S. R.; Shultz, N.; Siegler, M. A.; Smith, P. H.; Tatsumi, E.; Thomas, C. A.; Walsh, K. J.; Wolner, C. W. V.; Zou, X.-D. and Lauretta, D. S. (2019). Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis. Nature Astronomy, 3 pp. 341-351. For guidance on citations see FAQs.Length of main text: 2956 words Length of methods: 3605 words Length of legends: 565 words Number of references: 53 main text, 69 including methods and supplementary information (refs 67 to 69 are cited in the SI only) , we show that asteroid (101955) Bennu's surface is globally rough, dense with boulders and low in albedo. The number of boulders is surprising given Bennu's moderate thermal inertia, suggesting that simple models linking thermal inertia to particle size do not adequately capture the complexity relating these properties. At the same time, we find evidence for a wide range of particle sizes with distinct albedo characteristics. Our findings imply that ages of Bennu's surface particles span from the disruption of the asteroid's parent body (boulders) to recent in situ production (micron-scale particles).

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Section: Supplementary Materialsmentioning

confidence: 76%

Section: Spatially Resolved Surface Morphology and Boulder Distributionmentioning

confidence: 97%

Section: Spatially Resolved Surface Morphology and Boulder Distributionmentioning

confidence: 98%

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Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis

et al. 2019

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“…This technique relies on the assumption that all the particles were ejected from the exact same location and the approximation that the particle velocities remained constant after ejection. This constant velocity approximation is reasonable for fast‐moving particles observed soon after ejection given the weak gravity of Bennu, which has an average surface acceleration of 0.00006 m/s 2 (Barnouin et al, ; Scheeres et al, ). Traditional OD techniques using high‐fidelity force models allow for more accurate and precise particle trajectory and ejection location estimation, but our technique makes it possible to characterize all of the observed particle events, including those with too few observations for OD.…”

Section: Introductionmentioning

confidence: 88%

Reconstruction of Bennu Particle Events From Sparse Data

Pelgrift¹,

Lessac-Chenen²,

Adam³

et al. 2020

Earth and Space Science

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OSIRIS‐REx began observing particle ejection events shortly after entering orbit around near‐Earth asteroid (101955) Bennu in January 2019. For some of these events, the only observations of the ejected particles come from the first two images taken immediately after the event by OSIRIS‐REx's NavCam 1 imager. Without three or more observations of each particle, traditional orbit determination is not possible. However, by assuming that the particles all ejected at the same time and location for a given event, and approximating that their velocities remained constant after ejection (a reasonable approximation for fast‐moving particles, i.e., with velocities on the order of 10 cm/s or greater, given Bennu's weak gravity), we show that it is possible to estimate the particles' states from only two observations each. We applied this newly developed technique to reconstruct the particle ejection events observed by the OSIRIS‐REx spacecraft during orbit about Bennu. Particles were estimated to have ejected with inertial velocities ranging from 7 cm/s to 3.3 m/s, leading to a variety of trajectory types. Most (>80%) of the analyzed events were estimated to have originated from midlatitude regions and to have occurred after noon (local solar time), between 12:44 and 18:52. Comparison with higher‐fidelity orbit determination solutions for the events with sufficient observations demonstrates the validity of our approach and also sheds light on its biases. Our technique offers the capacity to meaningfully constrain the properties of particle ejection events from limited data.

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“…We assume that Phaethons structure is uniform because the internal condition is unknown. We consider three types of the bulk density, 0.5 g/cm 3 , 1.0 g/cm 3 , and 1.5 g/cm 3 , the averaged of which is consistent with that of a B-type asteroid (Scheeres et al 2019). Later, we denote the oblateness, the bulk density, and the gravitational constant as , ρ, and G, respectively.…”

Section: Semi-analytical Model For Structural Failure In a Top-shapedmentioning

confidence: 97%

Mass-shedding Activities of Asteroid (3200) Phaethon Enhanced by Its Rotation

Nakano

Hirabayashi

2020

ApJL

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Asteroid (3200) Phaethon, a B-type asteroid, has been active during its perihelion passages. This asteroid is considered to be a source of the Geminid meteor stream. It is reported that this asteroid is spinning at a rotation period of 3.60 hr and has a top shape (an oblate body with an equatorial ridge) with a mean equatorial diameter of 6.25 km. Here, we report that Phaethon's rotation state may be close to or above its critical rotation period when the bulk density is 0.5 − 1.5 g/cm 3 (a typical bulk density of a B-type asteroid). We found that in this condition, the structure of Phaethon is sensitive to failure unless the cohesive strength is ∼50 P a − ∼260 P a. This result implies that if there are some surface processes driven by, for example, thermal waves, large-scaled deformation may happen and cause mass shedding. From this interpretation, we propose the processes that produced the Geminid meteor stream in the past and dust tails recently. Phaethon initially rotated at a spin period shorter than the current period. The magnitude of structural deformation at this stage was higher than the present spin condition, and a large mass shedding event, i.e., the Geminid meteor stream, occurred. After this deformation process, the body became more oblate, and its spin slowed down. At this point, while the spin was high enough for the body to have mass shedding events, the magnitude of these events became small.

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The dynamic geophysical environment of (101955) Bennu based on OSIRIS-REx measurements

Abstract: The Open University's repository of research publications and other research outputs The dynamic geophysical environment of (101955) Bennu based on OSIRIS-REx measurements

Cited by 140 publications

References 35 publications

Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis

Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis

Reconstruction of Bennu Particle Events From Sparse Data

Mass-shedding Activities of Asteroid (3200) Phaethon Enhanced by Its Rotation

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