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Journal ArticleDOI

Near Earth Asteroids with measurable Yarkovsky effect

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.
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 ArticleDOI
Federica Spoto1, Federica Spoto2, Paolo Tanga1, Francois Mignard1  +498 moreInstitutions (86)
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.
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.

584 citations

Journal ArticleDOI
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.

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 ArticleDOI
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.

191 citations

Journal ArticleDOI
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.
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.

186 citations

Journal ArticleDOI
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.

171 citations

References
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Journal Article

75 citations


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

  • ...The Yarkovsky acceleration depends on several physical quantities such as spin state, size, mass, shape, and thermal properties (Vokrouhlický, 1999)....

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  • ...The Yarkovsky acceleration depends on several physical quantities such as spin state, size, mass, shape, and thermal properties (Vokrouhlický, 1999)....

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Journal ArticleDOI
01 Nov 2000-Icarus
TL;DR: In this article, the Earth crossing asteroid (ECA) 6489 Golevka (1991 JX) was observed using radar at Goldstone, the Very Large Array and the Evpatoria (Ukraine) and Kashima (Japan) radio antennas.

72 citations

Journal Article
TL;DR: In this article, a linear theory for the heat conduction in a spherical, solid and rotating body illuminated by solar radiation is developed in detail and the principal aim is to compute the recoil force, due to thermally reemitted radiation, which is commonly known as the Yarkovsky force.
Abstract: A linear theory for the heat conduction in a spherical, solid and rotating body illuminated by solar radiation is developed in detail. The principal aim is to compute the recoil force, due to thermally reemitted radiation, which is commonly known as the “Yarkovsky force”. We concentrate on the thermal effect which depends on the rotational period of a body rather than on the period of revolution around the Sun and deal with the general case of an arbitrary obliquity of the spin axis to the orbital plane. This “diurnal” thermal effect is considered to be an important source of mobility for meter-sized stony asteroidal fragments in the main belt. We compare our results with those of previous authors and show that the results of Peterson (1976) are accurate for meter-sized asteroidal bodies (although he used unrealistically long rotation periods).

71 citations


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

  • ...From Vokrouhlický (1998), we have at ≃ 4(1 − A) 9 Φ(r)f(Θ) cos γ , f(Θ) = 0.5Θ 1 + Θ + 0.5Θ2 (8) for the Yarkovsky diurnal component (which is typically dominant) , where A is the Bond albedo, Θ is the thermal parameter, γ is the obliquity, and 4 Φ(r) is the standard radiation force factor, which…...

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Journal ArticleDOI
01 Oct 2009-Icarus
TL;DR: In this paper, the authors present an analysis of the impact probability of the potentially hazardous Asteroid (101955) 1999 RQ 36 in the latter half of the 22nd century, well beyond the traditional 100-year time horizon for routine impact monitoring.

71 citations


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

  • ...These encounters transform a very well determined orbit into a poorly known one for which chaotic effects are dominant (Milani et al., 2009)....

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  • ...Milani et al. (2009) show how the size of the semimajor axis drift along with its uncertainty modifies impact predictions for the next century for 1999 RQ36....

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Journal ArticleDOI
01 Aug 1989-Icarus
TL;DR: In this paper, a full, least-squares adjustment of all ephemeris parameters, including the relevant asteroid masses, is compiled on the basis of observational data encompassing the highly accurate Viking Lander ranging data.

64 citations