The geophysical environment of Bennu

Scheeres, Daniel J.; Hesar, Siamak G.; Tardivel, Simon; Hirabayashi, Masatoshi; Farnocchia, Davide; McMahon, Jay W.; Chesley, S. R.; Barnouin, Olivier S.; Binzel, Richard P.; Bottke, W. F.; Daly, M. G.; Emery, Joshua P.; Hergenrother, C. W.; Лауретта, Д. С.; Marshall, John R.; Michel, Patrick; Nolan, M. C.; Walsh, K. J.

doi:10.1016/j.icarus.2016.04.013

Cited by 102 publications

(140 citation statements)

References 73 publications

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“…This measurement is opposite in direction and an order of magnitude smaller than the Normal YORP acceleration calculated by Scheeres et al (2016) but is consistent with the Normal plus Tangential YORP contribution. An acceleration of +2.64 ± 1.05 × 10 −6 deg/day 2 is needed, which indicates that Bennu's rotation rate has increased over the past two decades.…”

Section: Discussionsupporting

confidence: 83%

“…The present shape of Bennu is similar to other objects near the rotational stability limit Scheeres et al, 2016), suggesting that perhaps it was rotating faster in the past. Of particular interest is understanding the possible combination of Normal and Tangential YORP effects.…”

Section: Discussionsupporting

confidence: 76%

“…Using the radar shape model and associated pole and rotation rate, along with the homogeneous density estimate from Chesley et al (2014), Scheeres et al (2016) predicted the socalled Normal YORP acceleration for Bennu to be −15 × 10 −6 deg/day 2 . Using the radar shape model and associated pole and rotation rate, along with the homogeneous density estimate from Chesley et al (2014), Scheeres et al (2016) predicted the socalled Normal YORP acceleration for Bennu to be −15 × 10 −6 deg/day 2 .…”

Section: Mechanisms Of Accelerationmentioning

confidence: 99%

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Detection of Rotational Acceleration of Bennu Using HST Light Curve Observations

Nolan

Howell

Scheeres

et al. 2019

Geophysical Research Letters

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We observed the near‐Earth asteroid (101955) Bennu from the ground in 1999 and 2005, and with the Hubble Space Telescope (HST) in 2012, to constrain its rotation rate. The data reveal an acceleration of 2.64 ± 1.05 × 10−6 deg/day2, which could be due to a change in the moment of inertia of Bennu or to spin up from the Yarkovsky‐O'Keefe‐Radzievskii‐Paddack effect or other source of angular momentum. The best solution is within 1 σ of the period determined by Nolan et al. (2013, https://doi.org/10.1016/j.icarus.2013.05.028). The Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer (OSIRIS‐REx) mission will determine the rotation state independently in 2019. Those measurements should show whether the change in rotation rate is a steady increase (due, e.g., to the Yarkovsky‐O'Keefe‐Radzievskii‐Paddack effect) or some other phenomenon. The precise shape and surface properties measured by the OSIRIS‐REx science team will allow for a better understanding of variations in rotation rate of small asteroids.

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Section: Discussionsupporting

confidence: 83%

Section: Discussionsupporting

confidence: 76%

Section: Mechanisms Of Accelerationmentioning

confidence: 99%

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Detection of Rotational Acceleration of Bennu Using HST Light Curve Observations

Nolan

Howell

Scheeres

et al. 2019

Geophysical Research Letters

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“…In this paper, we are assuming that the body rotates uniformly with velocity ω, and the polyhedral model representing its shape is centred in the centre of mass and in aligned with the main axes of inertia. Then, the geopotential, in this case, takes the form (Scheeres et al 2016):…”

Section: Gravitational Field and Geopotentialmentioning

confidence: 99%

“…Then, the equations that determine the motion of a particle orbiting a body with uniform rotation on its axis of maximum moment of inertia are described as (Scheeres et al 2016):…”

Section: Equation Of Motionmentioning

confidence: 99%

Asteroid triple-system 2001 SN263: surface characteristics and dynamical environment

Winter

Valvano

Moura

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The (153591) 2001 SN 263 asteroid system, target of the first Brazilian interplanetary space mission, is one of the known three triple systems within the population of NEAs. One of the mission objectives is to collect data about the formation of this system. The analysis of these data will help in the investigation of the physical and dynamical structures of the components (Alpha, Beta and Gamma) of this system, in order to find vestiges related to its origin. In this work, we assume the irregular shape of the 2001 SN 263 system components as uniform density polyhedra and computationally investigate the gravitational field generated by these bodies. The goal is to explore the dynamical characteristics of the surface and environment around each component. Then, taking into account the rotational speed, we analyze their topographic features through the quantities geometric altitude, tilt, geopotential, slope, surface accelerations, among others. Additionally, the investigation of the environment around the bodies made it possible to construct zero-velocity curves, which delimit the location of equilibrium points. The Alpha component has a peculiar number of 12 equilibrium points, all of them located very close to its surface. In the cases of Beta and Gamma, we found four equilibrium points not so close to their surfaces. Then, performing numerical experiments around their equilibrium points, we identified the location and size of just one stable region, which is associated with an equilibrium point around Beta. Finally, we integrated a spherical cloud of particles around Alpha and identified the location on the surface of Alpha were the particles have fallen.

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Missions to the Asteroids

Vepa

2024

Space Vehicle Maneuvering, Propulsion, Dynamics and Control

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The geophysical environment of Bennu

Cited by 102 publications

References 73 publications

Detection of Rotational Acceleration of Bennu Using HST Light Curve Observations

Detection of Rotational Acceleration of Bennu Using HST Light Curve Observations

Asteroid triple-system 2001 SN263: surface characteristics and dynamical environment

Missions to the Asteroids

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