Near Earth Asteroids with measurable Yarkovsky effect

doi:10.1016/J.ICARUS.2013.02.004

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Near Earth Asteroids with measurable Yarkovsky effect

Journal Article•DOI•

Near Earth Asteroids with measurable Yarkovsky effect

Davide Farnocchia¹, Steven R. Chesley¹, David Vokrouhlický², Andrea Milani³, Federica Spoto³, William F. Bottke⁴ - Show less +2 more•Institutions (4)

Jet Propulsion Laboratory¹, Charles University in Prague², University of Pisa³, Southwest Research Institute⁴

01 May 2013-Icarus (Academic Press)-Vol. 224, Iss: 1, pp 1-13

TL;DR: In this article, the Yarkovsky effect among near Earth asteroids (NEAs) was investigated by measuring the YARKovsky-related orbital drift from the orbital fit using a high precision dynamical model, including the Newtonian attraction of 16 massive asteroids and the planetary relativistic terms.

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About: This article is published in Icarus.The article was published on 2013-05-01 and is currently open access. It has received 140 citations till now. The article focuses on the topics: Yarkovsky effect & Near-Earth object.

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Journal Article•DOI•

Gaia Data Release 2. Observations of solar system objects

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Federica Spoto¹, Federica Spoto², Paolo Tanga¹, Francois Mignard¹ +498 more•Institutions (86)

10 Aug 2018-Astronomy and Astrophysics

TL;DR: In this paper, the authors describe the processing of the Gaia DR2 data, and describe the criteria used to select the sample published in Gaia DR 2, and explore the data set to assess its quality.

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Abstract: Context. The Gaia spacecraft of the European Space Agency (ESA) has been securing observations of solar system objects (SSOs) since the beginning of its operations. Data Release 2 (DR2) contains the observations of a selected sample of 14,099 SSOs. These asteroids have been already identified and have been numbered by the Minor Planet Center repository. Positions are provided for each Gaia observation at CCD level. As additional information, complementary to astrometry, the apparent brightness of SSOs in the unfiltered G band is also provided for selected observations.Aims. We explain the processing of SSO data, and describe the criteria we used to select the sample published in Gaia DR2. We then explore the data set to assess its quality.Methods. To exploit the main data product for the solar system in Gaia DR2, which is the epoch astrometry of asteroids, it is necessary to take into account the unusual properties of the uncertainty, as the position information is nearly one-dimensional. When this aspect is handled appropriately, an orbit fit can be obtained with post-fit residuals that are overall consistent with the a-priori error model that was used to define individual values of the astrometric uncertainty. The role of both random and systematic errors is described. The distribution of residuals allowed us to identify possible contaminants in the data set (such as stars). Photometry in the G band was compared to computed values from reference asteroid shapes and to the flux registered at the corresponding epochs by the red and blue photometers (RP and BP).Results. The overall astrometric performance is close to the expectations, with an optimal range of brightness G ~ 12 − 17. In this range, the typical transit-level accuracy is well below 1 mas. For fainter asteroids, the growing photon noise deteriorates the performance. Asteroids brighter than G ~ 12 are affected by a lower performance of the processing of their signals. The dramatic improvement brought by Gaia DR2 astrometry of SSOs is demonstrated by comparisons to the archive data and by preliminary tests on the detection of subtle non-gravitational effects.

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584 citations

Journal Article•DOI•

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

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Steven R. Chesley¹, Davide Farnocchia¹, Michael C. Nolan², David Vokrouhlický³, Paul W. Chodas¹, Andrea Milani, Federica Spoto, Benjamin Rozitis⁴, Lance A. M. Benner¹, William F. Bottke⁵, Michael W. Busch⁶, Joshua P. Emery⁷, Ellen S. Howell², Dante S. Lauretta⁸, Jean-Luc Margot⁹, Patrick A. Taylor² - Show less +12 more•Institutions (9)

California Institute of Technology¹, Arecibo Observatory², Charles University in Prague³, Open University⁴, Southwest Research Institute⁵, Search for extraterrestrial intelligence⁶, University of Tennessee⁷, University of Arizona⁸, University of California, Los Angeles⁹

01 Jun 2014-Icarus

TL;DR: The OSIRIS-REx asteroid sample return mission target, (101955) Bennu (formerly 1999 RQ 36), is a half-kilometer near-Earth asteroid with an extraordinarily well constrained orbit as mentioned in this paper.

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238 citations

Cites background or methods from "Near Earth Asteroids with measurabl..."

...Given an estimated value of AT and the assumed value of d, one can readily derive the time-averaged da/dt using Gauss’ planetary equations (Farnocchia et al. 2013b)....
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...As the Yarkovsky induced orbital drift depends on the osculating orbital elements (Farnocchia et al. 2013b), there are also commensurable variations in the da/dt evolution (see Fig....
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...More recently Nugent et al. (2012) and Farnocchia et al. (2013b) have estimated the Yarkovsky effect for a few tens of near-Earth asteroids by using a formulation that depends on a single parameter to be determined from the orbital fit....
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...The orbital predictions and the impact hazard assessment are then performed by a Monte Carlo simulation that accounts for both the Yarkovsky effect distribution and the orbital uncertainty (Farnocchia et al. 2013a; Farnocchia and Chesley 2014)....
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...Importantly, it requires no information about the physical characteristics or spin state of the asteroid, and so it can be implemented readily in cases where only astrometric information is available (e.g., Vokrouhlický et al. 2008; Chesley et al. 2008; Nugent et al. 2012; Farnocchia et al. 2013b)....
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Journal Article•DOI•

Asteroid families classification: Exploiting very large datasets

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Andrea Milani¹, Alberto Cellino², Zoran Knežević, Bojan Novaković³, Federica Spoto¹, Paolo Paolicchi¹ - Show less +2 more•Institutions (3)

University of Pisa¹, INAF², University of Belgrade³

01 Sep 2014-Icarus

TL;DR: A new approach to the asteroid family classification by combining the Hierarchical Clustering Method (HCM) with a method to add new members to existing families, which allows to solve some difficult cases of families overlapping in the proper elements space but generated by different collisional events.

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191 citations

Journal Article•DOI•

Cohesive forces prevent the rotational breakup of rubble-pile asteroid (29075) 1950 DA

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Ben Rozitis¹, Eric M. MacLennan¹, Joshua P. Emery¹•Institutions (1)

University of Tennessee¹

14 Aug 2014-Nature

TL;DR: It is reported that the kilometre-sized asteroid (29075) 1950 DA is a rubble pile that is rotating faster than is allowed by gravity and friction and that the strengths of the forces are comparable to, though somewhat less than, the forces found between the grains of lunar regolith.

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Abstract: Modelling and observations of the kilometre-sized asteroid (29075) 1950 DA reveal it to be a ‘rubble pile’ that is rotating faster than is allowed by gravity and friction; cohesive forces such as those in lunar regolith are required to prevent it breaking up. Some asteroids are solid bodies but others, known as 'rubble-pile' asteroids, are loose aggregates of sand- to boulder-sized components. The conventional view, that rubble piles are held together by gravitational and frictional forces alone, has recently been questioned. It has been suggested that small van der Waals forces between constituent grains may be an important factor. Here, Ben Rozitis et al. report that the kilometre-sized rubble-pile asteroid (29075) 1950 DA is rotating faster than the breakup limit for its density calculated assuming the action of gravity and friction alone. They conclude that inter-particle cohesive forces must be holding the asteroid together and that the forces are comparable to, though somewhat less than, those found between the grains of lunar regolith. Space missions1 and ground-based observations2 have shown that some asteroids are loose collections of rubble rather than solid bodies. The physical behaviour of such ‘rubble-pile’ asteroids has been traditionally described using only gravitational and frictional forces within a granular material3. Cohesive forces in the form of small van der Waals forces between constituent grains have recently been predicted to be important for small rubble piles (ten kilometres across or less), and could potentially explain fast rotation rates in the small-asteroid population4,5,6. The strongest evidence so far has come from an analysis of the rotational breakup of the main-belt comet P/2013 R3 (ref. 7), although that was indirect and poorly constrained by observations. Here we report that the kilometre-sized asteroid (29075) 1950 DA (ref. 8) is a rubble pile that is rotating faster than is allowed by gravity and friction. We find that cohesive forces are required to prevent surface mass shedding and structural failure, and that the strengths of the forces are comparable to, though somewhat less than, the forces found between the grains of lunar regolith.

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186 citations

Journal Article•DOI•

Debiased orbit and absolute-magnitude distributions for near-Earth objects

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Mikael Granvik¹, Alessandro Morbidelli, Robert Jedicke, Bryce Bolin, William F. Bottke², E. C. Beshore³, David Vokrouhlický⁴, David Nesvorný², Patrick Michel - Show less +5 more•Institutions (4)

University of Helsinki¹, Southwest Research Institute², University of Arizona³, Charles University in Prague⁴

15 Sep 2018-Icarus

TL;DR: In this article, the authors presented a new four-dimensional model of the near-Earth objects population that describes debiased steady-state distributions of semimajor axis, eccentricity, inclination, and absolute magnitude H in the range 17.962 − 56 + 52 + 52 ( 802 − 42 + 48 × 10 3 ) NEOs with H.

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171 citations

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References

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Dissertation•DOI•

Surface Properties of Asteroids from Mid-Infrared Observations and Thermophysical Modeling

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Michael Müller

01 Jan 2007

TL;DR: The TPM for non-convex shapes of asteroids is proposed in this paper. But the authors do not discuss the future work of the TPM in this paper. And they do not provide a detailed thermophysical modeling of the model.

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Abstract: Title, Abstract, Contents Chapter 1: Introduction Chapter 2: Thermal emission of asteroids Chapter 3: Detailed thermophysical modeling Chapter 4: IRTF observations Chapter 5: Spitzer observations Chapter 6: Results Chapter 7: Discussion Chapter 8: Conclusions Chapter 9: Future work Appendix: TPM for non-convex shapes Bibliography Acknowledgments Zusammenfassung Publikationen, Selbstandigkeitserklarung

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38 citations

Journal Article•DOI•

Detection of radiation pressure acting on 2009 BD

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Marco Micheli¹, David J. Tholen¹, Garrett T. Elliott¹•Institutions (1)

University of Hawaii¹

01 May 2012-New Astronomy

TL;DR: In this paper, the authors reported the direct detection of radiation pressure on the asteroid 2009 BD, one of the smallest multi-opposition near-Earth objects currently known, with H ∼ 28.4.

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36 citations

"Near Earth Asteroids with measurabl..." refers background in this paper

...This results in an area to mass ratio A/M = (2.72 ± 0.39) × 10−4 m3/kg, which is consistent at the 1-σ level with the value reported by Micheli et al. (2012), i.e., (2.97 ± 0.33) × 10−4 m3/kg....
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...Micheli et al. (2012) show that including solar radiation pressure allows an improvement in the fit to the observations and the recovery of Mauna Kea observations....
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...Asteroid 2009 BD is very small and to fit its observational dataset it is necessary to include solar radiation pressure (Micheli et al., 2012)....
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Journal Article•DOI•

Radar observations and a physical model of Asteroid 4660 Nereus, a prime space mission target

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Marina Brozovic¹, Steven J. Ostro¹, Lance A. M. Benner¹, Jon D. Giorgini¹, Raymond F. Jurgens¹, Randy Rose¹, Michael C. Nolan², A. A. Hine², Christopher Magri³, Daniel J. Scheeres⁴, Jean-Luc Margot⁵ - Show less +7 more•Institutions (5)

California Institute of Technology¹, Arecibo Observatory², University of Maine at Farmington³, University of Colorado Boulder⁴, Cornell University⁵

01 May 2009-Icarus

TL;DR: In this article, an ellipsoid model of Nereus was used to estimate the rotation period of the near-Earth Asteroid 4660 NEAR NEAR NERUS during its 2002 close-approach.

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30 citations

Journal Article•

Orbit Uncertainties, Keyholes, and Collision Probabilities

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P. W. Chodas

10 Oct 1999-Bulletin of the American Astronomical Society

27 citations

"Near Earth Asteroids with measurabl..." refers background in this paper

...In both cases the Yarkovsky effect is large enough to shift the position at the scattering close approach by an amount much larger than the distance between the keyholes (Chodas, 1999) corresponding to impacts in later years (2036, 2037, 2068 for Apophis; 2175, 2180, 2196 for 1999 RQ36)....
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Journal Article•DOI•

The rotational poles and shapes of 1580 Betulia and 3908 (1980PA) from one apparition

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J. D. Drummond¹, Wieslaw Z. Wisniewski¹•Institutions (1)

University of Arizona¹

01 Feb 1990-Icarus

TL;DR: The rotational poles, triaxial ellipsoid shapes, absolute magnitudes, and phase functions of two Amor asteroids have been calculated from lightcurves obtained in a single apparition as discussed by the authors.

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17 citations