Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu

Chesley, Steven R.; Farnocchia, Davide; Nolan, M. C.; Vokrouhlický, David; Chodas, P. W.; Milani, Andrea; Spoto, F.; Rozitis, B.; Benner, L. A. M.; Bottke, W. F.; Busch, Michael W.; Emery, Joshua P.; Howell, E. S.; Лауретта, Д. С.; Margot, Jean-Luc; Taylor, Patrick A.

doi:10.1016/j.icarus.2014.02.020

Cited by 213 publications

(218 citation statements)

References 52 publications

Supporting

Mentioning

208

Contrasting

Order By: Relevance

“…These densities are not, a priori, unreasonable estimates for Bennu. Chesley et al (2013), obtain an estimate of the bulk density of the entire asteroid to be ~ 1 g cm -3 from a measurement of the Yarkovsky effect on the orbit of Bennu, suggesting a fairly uniform porosity of about 0.5 for the entire asteroid, though the uncertainties are large enough to prevent drawing any firm conclusions. More recent studies of the densities of L-chondrites (Consolmagno, Britt and Mackey, 2008) give slightly lower densities (by 5-10%), and the results should scale with that value.…”

Section: Near-surface Bulk Densitymentioning

confidence: 98%

“…Further radar observations obtained in September 2011 had too low a signal-to-noise ratio (SNR) to be useful for characterizing the shape of the asteroid. Chesley et al (2013) used them, along with the other observations reported here, for computing its orbit. The observations at Goldstone have lower (by a factor of about 20) SNR than the Arecibo images, but many were obtained at times when the object was not visible from Arecibo.…”

Section: Observationsmentioning

confidence: 99%

See 1 more Smart Citation

Shape model and surface properties of the OSIRIS-REx target Asteroid (101955) Bennu from radar and lightcurve observations

Nolan

Magri

Howell

et al. 2013

Icarus

Self Cite

206

214

View full text Add to dashboard Cite

We determine the three-dimensional shape of near-Earth asteroid (101955) Bennu based on radar images and optical lightcurves. Bennu was observed both in 1999 at its discovery apparition, and in 2005 using the 12.6-cm radar at the Arecibo Observatory and the 3.5-cm radar at the Goldstone tracking station. Data obtained in both apparitions were used to construct a shape model of this object. Observations were also obtained at many other wavelengths to characterize this object, some of which were used to further constrain the shape modeling (Clark et al., 2011;Hergenrother et al., 2013; Krugly et al., 1999). The lightcurve data, along with an initial determination of the rotation period derived from them, simplified and improved the shape modeling.Below we briefly describe the observations and shape modeling process. We discuss the shape model and the implications for the possible formation and evolution of this object. We also describe the importance and limitations of the shape model in view of the fact that this object is the target of the OSIRIS-REx spacecraft mission.

show abstract

Section: Near-surface Bulk Densitymentioning

confidence: 98%

Section: Observationsmentioning

confidence: 99%

Shape model and surface properties of the OSIRIS-REx target Asteroid (101955) Bennu from radar and lightcurve observations

Nolan

Magri

Howell

et al. 2013

Icarus

Self Cite

206

214

View full text Add to dashboard Cite

show abstract

“…APPENDIX A: PHYSICAL PARAMETERS OF ASTEROID (101955) BENNU Table 6 summarizes the relevant physical parameters for Bennu [30]. Surface emissivity: 0.90 ± 0.05…”

Section: Acknowledgementmentioning

confidence: 99%

Precise Model for Small-Body Thermal Radiation Pressure Acting on Spacecraft

Hesar

Scheeres

McMahon

et al. 2017

Journal of Guidance, Control, and Dynamics

Self Cite

View full text Add to dashboard Cite

A precise representation of small body surface thermal radiation pressure effects acting on orbiting spacecraft is discussed. The proposed framework takes advantage of a general Fourier series expansion to compute small body surface thermal radiation pressure. Fourier series expansion has been used before for the precise representation of solar radiation pressure effects on spacecraft orbiting small bodies. This framework takes into account the surface thermal parameters of small bodies, geometric relationship of orbiting spacecraft with the small body surface, and the shape and surface properties of spacecraft allowing for the computation of thermal radiation pressure, which may also be used for the generation of precise orbit determination solutions.After presenting the general model, we provide an example application of the model for the OSIRIS-REx spacecraft in orbit about Asteroid (101955) Bennu. Via simulation studies, we evaluate the effect of mis-modeling the thermal radiation pressure on the spacecraft and study the utilization of the proposed method for generating precise orbit determination solutions.

show abstract

“…In particular, the Yarkovsky effect could explain the transportation of asteroids from the main belt region to the inner solar system (Bottke et al 2006). It also becomes necessary for accurate orbit determination or prediction of trajectory of near-Earth asteroids (NEA), in particular, in the context of close approach or impact predictions (Farnocchia et al 2013a;Chesley et al 2014). …”

Section: Introductionmentioning

confidence: 99%

Detection of Yarkovsky acceleration in the context of precovery observations and the futureGaiacatalogue

Desmars

2015

A&A

View full text Add to dashboard Cite

Context. The Yarkovsky effect is a weak non-gravitational force leading to a small variation of the semi-major axis of an asteroid. Using radar measurements and astrometric observations, it is possible to measure a drift in semi-major axis through orbit determination. Aims. This paper aims to detect a reliable drift in semi-major axis of near-Earth asteroids (NEAs) from ground-based observations and to investigate the impact of precovery observations and the future Gaia catalogue in the detection of a secular drift in semi-major axis. Methods. We have developed a precise dynamical model of an asteroid's motion taking the Yarkovsky acceleration into account and allowing the fitting of the drift in semi-major axis. Using statistical methods, we investigate the quality and the robustness of the detection. Results. By filtering spurious detections with an estimated maximum drift depending on the asteroid's size, we found 46 NEAs with a reliable drift in semi-major axis in good agreement with the previous studies. The measure of the drift leads to a better orbit determination and constrains some physical parameters of these objects. Our results are in good agreement with the 1/D dependence of the drift and with the expected ratio of prograde and retrograde NEAs. We show that the uncertainty of the drift mainly depends on the length of orbital arc and in this way we highlight the importance of the precovery observations and data mining in the detection of consistent drift. Finally, we discuss the impact of Gaia catalogue in the determination of drift in semi-major axis.

show abstract

Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu

Cited by 213 publications

References 52 publications

Shape model and surface properties of the OSIRIS-REx target Asteroid (101955) Bennu from radar and lightcurve observations

Shape model and surface properties of the OSIRIS-REx target Asteroid (101955) Bennu from radar and lightcurve observations

Precise Model for Small-Body Thermal Radiation Pressure Acting on Spacecraft

Detection of Yarkovsky acceleration in the context of precovery observations and the futureGaiacatalogue

Contact Info

Product

Resources

About