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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Journal Article•DOI•

Keck observations of near-Earth asteroids in the thermal infrared

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Marco Delbo, Alan W. Harris, Richard P. Binzel¹, Petr Pravec², John K. Davies³ - Show less +1 more•Institutions (3)

Massachusetts Institute of Technology¹, Academy of Sciences of the Czech Republic², UK Astronomy Technology Centre³

01 Nov 2003-Icarus

TL;DR: In this article, the results of thermal-infrared observations of 20 near-Earth asteroids (NEAs) obtained in the period March 2000-February 2002 with the 10m Keck-I telescope on Mauna Kea, Hawaii were presented.

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171 citations

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

...The rectangles correspond to reasonable values of q according to the taxonomic type and to a reasonable range of C (Delbó et al., 2007). D. Farnocchia et al. / Icarus 224 (2013) 1–13 11...
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...According to Delbó et al. (2003) Ra-Shalom has an unusually high thermal inertia....
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Journal Article•DOI•

Yarkovsky Effect on Small Near-Earth Asteroids: Mathematical Formulation and Examples

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David Vokrouhlický¹, David Vokrouhlický², David Vokrouhlický³, Andrea Milani¹, Andrea Milani³, Andrea Milani², S. R. Chesley¹, S. R. Chesley³, S. R. Chesley² - Show less +5 more•Institutions (3)

Charles University in Prague¹, California Institute of Technology², University of Pisa³

01 Nov 2000-Icarus

TL;DR: In this article, the authors investigated the possibility of detecting the Yarkovsky effect via precise orbit determination of near-Earth asteroids, which is feasible only with the existence of precise radar astrometry at multiple apparitions.

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153 citations

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

...Typical values of da/dt for sub-kilometer NEAs are 10 (4)–10 3 au/Myr (Vokrouhlický et al., 2000)....
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...The diurnal Yarkovsky effect produces a semimajor axis drift proportional to cosc (Vokrouhlický et al., 2000)....
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...The diurnal Yarkovsky effect produces a semimajor axis drift proportional to cos γ (Vokrouhlický et al., 2000)....
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...As the seasonal component is typically 10 times smaller then the diurnal one (Vokrouhlický et al., 2000) we mark this detection as spurious....
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...…important nongravitational perturbation is the Yarkovsky effect, which is due to radiative recoil of anisotropic thermal emission and causes asteroids to undergo a secular semimajor axis drift da/dt. Typical values of da/dt for sub-kilometer NEAs are 10−4–10−3 au/Myr (Vokrouhlický et al., 2000)....
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Journal Article•DOI•

Predicting the Earth encounters of (99942) Apophis

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Jon D. Giorgini¹, Lance A. M. Benner¹, Steven J. Ostro¹, Michael C. Nolan², Michael W. Busch¹ - Show less +1 more•Institutions (2)

California Institute of Technology¹, Arecibo Observatory²

01 Jan 2008-Icarus

TL;DR: In this article, the authors developed position uncertainty intervals to compensate for this by characterizing the minimum and maximum effect of physical parameters on the trajectory of Apophis' trajectory, and found no future small-body encounters likely to yield an apophis mass determination prior to 2029.

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137 citations

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

...According to Giorgini et al. (2002), the 2880 impact is ruled out by retrograde rotation....
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...Though only a marginal da/dt estimate is available, Giorgini et al. (2008) and Chesley et al. (2009) prove that the occurrence of an impact in 2036 is decisively driven by the magnitude of the Yarkovsky effect....
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Journal Article•DOI•

Astrometric masses of 26 asteroids and observations on asteroid porosity

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James Baer¹, Steven R. Chesley², Robert Matson³•Institutions (3)

James Cook University¹, California Institute of Technology², Science Applications International Corporation³

22 Mar 2011-The Astronomical Journal

TL;DR: In this article, the astrometric masses of 26 main-belt asteroids were estimated using an observational error model and an integrated ephemeris of 300 large asteroids, which was used in the mass determination algorithm to model significant perturbations from the rest of the main belt.

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Abstract: As an application of our recent observational error model, we present the astrometric masses of 26 main-belt asteroids. We also present an integrated ephemeris of 300 large asteroids, which was used in the mass determination algorithm to model significant perturbations from the rest of the main belt. After combining our mass estimates with those of other authors, we study the bulk porosities of over 50 main-belt asteroids and observe that asteroids as large as 300 km in diameter may be loose aggregates. This finding may place specific constraints on models of main-belt collisional evolution. Additionally, we observe that C-group asteroids tend to have significantly higher macroporosity than S-group asteroids.

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129 citations

Journal Article•DOI•

Retrograde spins of near-Earth asteroids from the Yarkovsky effect.

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A. La Spina¹, Paolo Paolicchi¹, Agnieszka Kryszczyńska², Petr Pravec•Institutions (2)

University of Pisa¹, Adam Mickiewicz University in Poznań²

25 Mar 2004-Nature

TL;DR: It is reported that the spin vectors of NEAs show a strong and statistically significant excess of retrograde rotations, quantitatively consistent with the theoretical expectations of the Yarkovsky model.

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Abstract: Dynamical resonances in the asteroid belt are the gateway for the production of near-Earth asteroids (NEAs). To generate the observed number of NEAs, however, requires the injection of many asteroids into those resonant regions. Collisional processes have long been claimed as a possible source, but difficulties with that idea have led to the suggestion that orbital drift arising from the Yarkovsky effect dominates the injection process. (The Yarkovsky effect is a force arising from differential heating-the 'afternoon' side of an asteroid is warmer than the 'morning' side.) The two models predict different rotational properties of NEAs: the usual collisional theories are consistent with a nearly isotropic distribution of rotation vectors, whereas the 'Yarkovsky model' predicts an excess of retrograde rotations. Here we report that the spin vectors of NEAs show a strong and statistically significant excess of retrograde rotations, quantitatively consistent with the theoretical expectations of the Yarkovsky model.

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107 citations

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

...Namely, we used the Einstein– Infeld–Hoffman (EIH) approximation as described in Moyer (2003) or Will (1993)....
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...Thus, the retrograde fraction should be 0.37+0.5×0.63 = 0.69, while La Spina et al. (2004) report 67% retrograde for their sample, which is dominated by large NEAs....
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...Namely, we used the Einstein– Infeld–Hoffman (EIH) approximation as described in Moyer (2003) or Will (1993). As already noted in Chesley et al....
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...La Spina et al. (2004) point out that this implies 37% of NEAs have retrograde spin (via ν6), plus half of the complement (via other pathways)....
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...However, we find it interesting that it appears to be consistent with the observed obliquity distribution of the NEAs (La Spina et al., 2004)....
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