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•

Coupled Spin and Shape Evolution of Small Rubble-pile Asteroids: Self-limitation of the YORP Effect

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Desireé Cotto-Figueroa¹, Desireé Cotto-Figueroa², Thomas S. Statler¹, Thomas S. Statler³, Thomas S. Statler⁴, Derek C. Richardson³, Paolo Tanga⁵ - Show less +3 more•Institutions (5)

Ohio University¹, Arizona State University², University of Maryland, College Park³, National Science Foundation⁴, University of Nice Sophia Antipolis⁵

09 Apr 2015-The Astrophysical Journal

TL;DR: In this article, the first selfconsistent simulations of the coupled spin-shape evolution of small gravitational aggregates under the influence of the YORP effect were presented, where the authors conjecture that self-limitation may inhibit formation of top-shapes, binaries, or both, by restricting the amount of angular momentum imparted to a deformable body.

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Abstract: We present the first self-consistent simulations of the coupled spin-shape evolution of small gravitational aggregates under the influence of the YORP effect. Because of YORP’s sensitivity to surface topography, even small centrifugally driven reconfigurations of aggregates can alter the YORP torque dramatically, resulting in spin evolution that can differ qualitatively from the rigid-body prediction. One-third of our simulations follow a simple evolution described as a modified YORP cycle. Two-thirds exhibit one or more of three distinct behaviors— stochastic YORP, self-governed YORP, and stagnating YORP—which together result in YORP self-limitation. Selflimitation confines rotation rates of evolving aggregates to far narrower ranges than those expected in the classical YORP cycle, greatly prolonging the times over which objects can preserve their sense of rotation. Simulated objects are initially randomly packed, disordered aggregates of identical spheres in rotating equilibrium, with low internal angles of friction. Their shape evolution is characterized by rearrangement of the entire body, including the deep interior. They do not evolve to axisymmetric top shapes with equatorial ridges. Mass loss occurs in one-third of the simulations, typically in small amounts from the ends of a prolate-triaxial body. We conjecture that YORP self-limitation may inhibit formation of top-shapes, binaries, or both, by restricting the amount of angular momentum that can be imparted to a deformable body. Stochastic YORP, in particular, will affect the evolution of collisional families whose orbits drift apart under the influence of Yarkovsky forces, in observable ways.

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55 citations

Journal Article•DOI•

Constraining the physical properties of Near-Earth object 2009 BD

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Michael Mommert¹, Joseph L. Hora², Davide Farnocchia³, S. Chesley³, David Vokrouhlický⁴, David E. Trilling¹, Michael Mueller, Alan W. Harris, Howard A. Smith², Giovanni G. Fazio² - Show less +6 more•Institutions (4)

Northern Arizona University¹, Harvard University², California Institute of Technology³, Charles University in Prague⁴

10 May 2014-The Astrophysical Journal

TL;DR: In this article, an upper-limit flux density determination from the Spitzer Space Telescope Infrared Array Camera observations of near-Earth object 2009 BD was performed in support of the NASA Asteroid Robotic Retrieval Mission concept.

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Abstract: We report on Spitzer Space Telescope Infrared Array Camera observations of near-Earth object 2009 BD that were carried out in support of the NASA Asteroid Robotic Retrieval Mission concept. We did not detect 2009 BD in 25 hr of integration at 4.5 μm. Based on an upper-limit flux density determination from our data, we present a probabilistic derivation of the physical properties of this object. The analysis is based on the combination of a thermophysical model with an orbital model accounting for the non-gravitational forces acting upon the body. We find two physically possible solutions. The first solution shows 2009 BD as a 2.9 ± 0.3 m diameter rocky body (ρ = 2.9 ± 0.5 g cm–3) with an extremely high albedo of that is covered with regolith-like material, causing it to exhibit a low thermal inertia ( SI units). The second solution suggests 2009 BD to be a 4 ± 1 m diameter asteroid with that consists of a collection of individual bare rock slabs (Γ = 2000 ± 1000 SI units, g cm–3). We are unable to rule out either solution based on physical reasoning. 2009 BD is the smallest asteroid for which physical properties have been constrained, in this case using an indirect method and based on a detection limit, providing unique information on the physical properties of objects in the size range smaller than 10 m.

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51 citations

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

...As the negative value of A2 suggests a retrograde rotation (see Farnocchia et al. 2013), we sample the obliquity γ from 90◦ to 180◦....
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...…forces is based on work done by Vokrouhlický et al. (2000), which is used to describe the Yarkovsky effect observed in a number of objects (e.g., Chesley et al. 2003; Vokrouhlický et al. 2008; Farnocchia et al. 2013; Chesley et al. 2014; Farnocchia and Chesley 2014; Farnocchia et al. 2014b)....
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Journal Article•DOI•

Asteroid clusters similar to asteroid pairs

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Petr Pravec¹, P. Fatka¹, P. Fatka², David Vokrouhlický², Daniel J. Scheeres³, Peter Kusnirak¹, Kamil Hornoch¹, Adrian Galad¹, J. Vrastil¹, J. Vrastil², Donald P. Pray, Yu. N. Krugly⁴, N. M. Gaftonyuk, R. Ya. Inasaridze⁵, V. R. Ayvazian⁵, O. Kvaratskhelia⁵, V. Zhuzhunadze⁵, Marek Husárik⁶, Walter R. Cooney, John Gross, Dirk Terrell⁷, Jozef Vilagi, Leonard Kornoš, Štefan Gajdoš, O. A. Burkhonov, Sh. A. Ehgamberdiev, Z. Donchev⁸, Galin Borisov⁸, Tanyu Bonev⁸, Vasilij Rumyantsev, Igor Molotov⁹ - Show less +27 more•Institutions (9)

Academy of Sciences of the Czech Republic¹, Charles University in Prague², University of Colorado Boulder³, University of Kharkiv⁴, Abastumani Astrophysical Observatory⁵, Slovak Academy of Sciences⁶, Southwest Research Institute⁷, Bulgarian Academy of Sciences⁸, Keldysh Institute of Applied Mathematics⁹

01 Apr 2018-Icarus

TL;DR: In this paper, Pravec et al. studied the membership, size ratio and rotational properties of 13 asteroid clusters consisting of between 3 and 19 known members that are on similar heliocentric orbits.

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47 citations

Journal Article•DOI•

The Yarkovsky effect for 99942 Apophis

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David Vokrouhlický¹, Davide Farnocchia², D. Čapek³, Steven R. Chesley², Petr Pravec³, P. Scheirich³, Thomas G. Müller⁴ - Show less +3 more•Institutions (4)

Charles University in Prague¹, California Institute of Technology², Academy of Sciences of the Czech Republic³, Max Planck Society⁴

15 May 2015-Icarus

TL;DR: In this article, the authors used the recently determined rotation state, shape, size and thermophysical model of Apophis to predict the strength of the Yarkovsky effect in its orbit.

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46 citations

Journal Article•DOI•

Assessment of the 2880 impact threat from Asteroid (29075) 1950 DA

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Davide Farnocchia¹, S. R. Chesley¹•Institutions (1)

California Institute of Technology¹

01 Feb 2014-Icarus

TL;DR: In this paper, the authors performed an assessment of the 2880 Earth impact risk for Asteroid (29075) 1950 DA using the contribution of the observational dataset and the astrometric treatment, the numerical error in long-term integration, and the different accelerations acting on the asteroid.

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45 citations

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References

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Book•

Theory and Experiment in Gravitational Physics

[...]

Clifford M. Will¹•Institutions (1)

Washington University in St. Louis¹

01 Jan 1981

TL;DR: In this paper, the authors provide a complete treatment of techniques for analyzing gravitation theory and experience, taking into account the Dicke framework, basic criteria for the viability of a gravitation theories, experimental tests of the Einstein equivalence principle, Schiff's conjecture, and a model theory devised by Lightman and Lee (1973).

...read moreread less

Abstract: New technological advances have made it feasible to conduct measurements with precision levels which are suitable for experimental tests of the theory of general relativity. This book has been designed to fill a new need for a complete treatment of techniques for analyzing gravitation theory and experience. The Einstein equivalence principle and the foundations of gravitation theory are considered, taking into account the Dicke framework, basic criteria for the viability of a gravitation theory, experimental tests of the Einstein equivalence principle, Schiff's conjecture, and a model theory devised by Lightman and Lee (1973). Gravitation as a geometric phenomenon is considered along with the parametrized post-Newtonian formalism, the classical tests, tests of the strong equivalence principle, gravitational radiation as a tool for testing relativistic gravity, the binary pulsar, and cosmological tests.

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1,692 citations

Journal Article•DOI•

Debiased Orbital and Absolute Magnitude Distribution of the Near-Earth Objects

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William F. Bottke¹, Alessandro Morbidelli, Robert Jedicke², Jean-Marc Petit, Harold F. Levison¹, Patrick Michel, Travis S. Metcalfe³ - Show less +3 more•Institutions (3)

Southwest Research Institute¹, University of Arizona², University of Texas at Austin³

01 Apr 2002-Icarus

TL;DR: In this article, a best-fit model of the near-Earth objects (NEOs) population is presented, which is fit to known NEs discovered or accidentally rediscovered by Spacewatch.

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717 citations

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

...This excess of retrograde rotators can be explained by the nature of resonance feeding into the inner Solar System (Bottke et al., 2002). Most of the primary NEA source regions (e.g., the 3:1 resonance, JFCs, Outer Belt, etc.) allow main belt asteroids to enter by drifting either inwards or outwards, but the m6 resonance is at the inner edge of the main belt and so asteroids can generally enter only by inwards drift, i.e., with retrograde rotation. Bottke et al. (2002) report that 37% of NEAs with absolute magnitude H < 22 arrive via m6 resonance. La Spina et al. (2004) point out that this implies 37% of NEAs have retrograde spin (via m6), plus half of the complement (via other pathways). 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. Table 2 contains 81% retrograde rotators, which is larger than 69% and thus, at face value, appears to be inconsistent with the theory. The sample of asteroids shown in Table 2, however, is based on measured Yarkovsky mobility and is not a representative sample of the debiased NEA population as described by Bottke et al. (2002). For example, the sample is dominated by small PHAs (MOID < 0.05 AU) on fairly deep Earth-crossing orbits. We find that 9 of the 21 objects are Aten asteroids (43%), compared to the 6% fraction predicted for the debiased NEA population. Bottke et al. (2002) suggest that the majority of Atens ( 79%) should come from the innermost region of the main belt where the m6 resonance is located....
[...]
...This excess of retrograde rotators can be explained by the nature of resonance feeding into the inner Solar System (Bottke et al., 2002)....
[...]
...This excess of retrograde rotators can be explained by the nature of resonance feeding into the inner Solar System (Bottke et al., 2002). Most of the primary NEA source regions (e.g., the 3:1 resonance, JFCs, Outer Belt, etc.) allow main belt asteroids to enter by drifting either inwards or outwards, but the m6 resonance is at the inner edge of the main belt and so asteroids can generally enter only by inwards drift, i.e., with retrograde rotation. Bottke et al. (2002) report that 37% of NEAs with absolute magnitude H < 22 arrive via m6 resonance....
[...]
...This excess of retrograde rotators can be explained by the nature of resonance feeding into the inner Solar System (Bottke et al., 2002). Most of the primary NEA source regions (e.g., the 3:1 resonance, JFCs, Outer Belt, etc.) allow main belt asteroids to enter by drifting either inwards or outwards, but the m6 resonance is at the inner edge of the main belt and so asteroids can generally enter only by inwards drift, i.e., with retrograde rotation. Bottke et al. (2002) report that 37% of NEAs with absolute magnitude H < 22 arrive via m6 resonance. La Spina et al. (2004) point out that this implies 37% of NEAs have retrograde spin (via m6), plus half of the complement (via other pathways). 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. Table 2 contains 81% retrograde rotators, which is larger than 69% and thus, at face value, appears to be inconsistent with the theory. The sample of asteroids shown in Table 2, however, is based on measured Yarkovsky mobility and is not a representative sample of the debiased NEA population as described by Bottke et al. (2002). For example, the sample is dominated by small PHAs (MOID < 0....
[...]
...Bottke et al. (2002) report that 37% of NEAs arrive via ν6 resonance....
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Journal Article•DOI•

THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics

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William F. Bottke¹, David Parry Rubincam•Institutions (1)

Southwest Research Institute¹

28 Apr 2006-Annual Review of Earth and Planetary Sciences

TL;DR: The Yarkovsky and YORP effects are thermal radiation forces and torques that cause small objects to undergo semimajor axis drift and spin vector modifications, respectively, as a function of their spin, orbit, and material properties as discussed by the authors.

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Abstract: The Yarkovsky and YORP (Yarkovsky-O’Keefe-Radzievskii-Paddack) effects are thermal radiation forces and torques that cause small objects to undergo semimajor axis drift and spin vector modifications, respectively, as a function of their spin, orbit, and material properties. These mechanisms help to (a) deliver asteroids (and meteoroids) with diameter D < 40 km from their source locations in the main belt to chaotic resonance zones capable of transporting this material to Earth-crossing orbits; (b) disperse asteroid families, with drifting bodies jumping or becoming trapped in mean-motion and secular resonances within the main belt; (c) modify the rotation rates and obliquities of D < 40 km asteroids; and (d ) allow asteroids to enter into spin-orbit resonances, which affect the evolution of their spin vectors and feedback into the Yarkovsky-driven semimajor axis evolution. Accordingly, we suggest that nongravitational forces should now be considered as important as collisions and gravitational perturbations to our overall understanding of asteroid evolution.

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661 citations

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

...It is well known that nongravitational forces should be considered as important as collisions and gravitational perturbations for the overall understanding of asteroid evolution (Bottke et al., 2006)....
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Application of photometric models to asteroids.

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Edward Bowell¹, Bruce Hapke, Deborah Domingue², Kari Lumme, Jouni Peltoniemi³, Alan W. Harris - Show less +2 more•Institutions (3)

Lowell Observatory¹, University of Pittsburgh², University of Helsinki³

01 Jan 1989

TL;DR: In this paper, the brightness of a rough and porous surface is parameterized in terms of the optical properties of individual particles, by shadowing between particles, and by the way in which light is scattered among collections of particles.

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Abstract: The way an asteroid or other atmosphereless solar system body varies in brightness in response to changing illumination and viewing geometry depends in a very complicated way on the physical and optical properties of its surface and on its overall shape. This paper summarizes the formulation and application of recent photometric models by Hapke (1981, 1984, 1986) and by Lumme and Bowell (1981). In both models, the brightness of a rough and porous surface is parameterized in terms of the optical properties of individual particles, by shadowing between particles, and by the way in which light is scattered among collections of particles. Both models succeed in their goal of fitting the observed photometric behavior of a wide variety of bodies, but neither has led to a very complete understanding of the properties of asteroid regoliths, primarily because, in most cases, the parameters in the present models cannot be adequately constrained by observations of integral brightness alone over a restricted range of phase angles.

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480 citations

Book•

Formulation for Observed and Computed Values of Deep Space Network Data Types for Navigation

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Theodore D. Moyer

31 Jan 2003

TL;DR: In this paper, the authors present algorithms for computing ET-TAI, including the calculation of precision light times and quasar delays, as well as partial derivatives of light times.

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Abstract: Foreword. Preface. Acknowledgments. Introduction. Time Scales and Time Differences. Planetary Ephemeris, Small-Body Ephemeris, and Satellite Ephemerides. Spacecraft Ephemeris and Partials File. Geocentric Space-Fixed Position, Velocity, and Acceleration Vectors of Tracking Station. Space-Fixed Position, Velocity, and Acceleration Vectors of a Landed Spacecraft Relative to Center of Mass of Planet, Planetary System, or the Moon. Algorithms for Computing ET-TAI. Light-Time Solution. Angles. Media and Antenna Corrections. Calculation of Precision Light Times and Quasar Delays. Partial Derivatives of Precision Light Times and Quasar Delays. Observables. References. Acronyms. Index.

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364 citations