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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Yarkovsky and YORP Effects in Dynamics of Small Bodies of the Solar System

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Jindřich Žižka

18 Sep 2018

TL;DR: In this paper, the influence of non-gravitational perturbations induced by the Yarkovsky/YORP effect and solar radiation pressure (SRP) on the orbital evolution of selected asteroids, asteroid families and pairs was studied.

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Abstract: In this thesis, we study the influence of non-gravitational perturbations induced by the Yarkovsky/YORP effect and solar radiation pressure (SRP) on the orbital evolution of selected asteroids, asteroid families and pairs. These perturbations are of great importance if one wants to perform precise and longterm propagation of meter-sized and kilometer-sized bodies. Although they have found many applications in the Solar System, here, we particularly investigated how they influence the orbit of near-Earth asteroid (99942) Apophis and what is their role in the age determination of asteroid families and pairs. Our numerical simulations showed that the perturbations of Apophis’ orbit caused by the SRP are orders of magnitude smaller than those produced by the Yarkovsky effect. The age determination of asteroid families and pairs was another pillar of this work. Over the past decade it turned out that the Yarkovsky effect must be taken into account for backward propagation of pair/family members. We modified the current method for estimating the age of asteroid pairs to be suitable for weakly convergent cases and discovered 7 young pairs with similar-sized components, which is in contradiction with the current theory of pair formation. In addition, we focused on an interesting pair of asteroids (87887) 2000 SS286 and (415992) 2002 AT49. This pair had ambiguous solution of its age. Nevertheless, using numerical experiments with synthetic pairs, we were able to determine its correct age and found that it is currently the youngest known system. Last but not least we constrained the age of the well-known pair (6070) Rheinland – (54827) 2001 NQ8 and determined the most probable rotational sense of (54827) 2001 NQ8.

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11 citations

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

...To make a preliminary test if and to what extent the Yarkovsky effect influences the orbital evolution of an asteroid, its available astrometric data is fitted using an additional transversal component of acceleration aT = A2/r(2), where r is the heliocentric distance (Farnocchia et al., 2013b)....
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...To make a preliminary test if and to what extent the Yarkovsky effect influences the orbital evolution of an asteroid, its available astrometric data is fitted using an additional transversal component of acceleration aT = A2/r2, where r is the heliocentric distance (Farnocchia et al., 2013b)....
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...With time, the number of successful detections grew, as well as the number of suspected cases, for which it might be possible to detect the Yarkovsky effect in future (Chesley et al., 2008; Nugent et al., 2012; Farnocchia et al., 2013b)....
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...The smallest body, for which the Yarkovsky effect was detected is 2009 BD (D ≈ 4 m), among the largest are (2100) Ra-Shalom and (4179) Toutatis (Nugent et al., 2012; Farnocchia et al., 2013b)....
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Journal Article•DOI•

Prospects of Dynamical Determination of General Relativity Parameter β and Solar Quadrupole Moment {J}_{2\odot } with Asteroid Radar Astronomy

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Ashok Kumar Verma, Jean-Luc Margot, Adam H. Greenberg

23 Aug 2017-The Astrophysical Journal

TL;DR: Verma et al. as mentioned in this paper evaluated the prospects of quantifying the parameterized post-Newtonian parameter beta and solar quadrupole moment J2 with observations of near-Earth asteroids with large orbital precession rates.

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Abstract: Author(s): Verma, Ashok K; Margot, Jean-Luc; Greenberg, Adam H | Abstract: We evaluated the prospects of quantifying the parameterized post-Newtonian parameter beta and solar quadrupole moment J2 with observations of near-Earth asteroids with large orbital precession rates (9 to 27 arcsec century$^{-1}$). We considered existing optical and radar astrometry, as well as radar astrometry that can realistically be obtained with the Arecibo planetary radar in the next five years. Our sensitivity calculations relied on a traditional covariance analysis and Monte Carlo simulations. We found that independent estimates of beta and J2 can be obtained with precisions of $6\times10^{-4}$ and $3\times10^{-8}$, respectively. Because we assumed rather conservative observational uncertainties, as is the usual practice when reporting radar astrometry, it is likely that the actual precision will be closer to $2\times10^{-4}$ and $10^{-8}$, respectively. A purely dynamical determination of solar oblateness with asteroid radar astronomy may therefore rival the helioseismology determination.

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9 citations

Journal Article•DOI•

Chasing the chelyabinsk asteroid n-body style

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C. de la Fuente Marcos, R. de la Fuente Marcos, Sverre J. Aarseth¹•Institutions (1)

University of Cambridge¹

06 Oct 2015-The Astrophysical Journal

TL;DR: In this article, a full N-body approach was used to compute a new orbital solution with an impact probability > 0.99999 and uncertainties in time and space of 0.2 s and 6 km.

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Abstract: On 2013 February 15 a small asteroid rammed against the atmosphere above the region of Chelyabinsk in Russia, producing the most powerful superbolide since the Tunguska event in 1908. Lacking proper astrometric observations, the pre-impact orbit of this object has been determined using videos, satellite images, and pure geometry. Unfortunately, more than two years after the event, the published estimates vary so much that there is no clear orbital solution that could be used to investigate the origin of the impactor and the existence of dynamically, or perhaps even genetically, related asteroids. Here, we revisit this topic using a full N-body approach. A robust statistical test is applied to published solutions to discard those unable to produce a virtual impact at the observed time (03:20:20.8 s UTC). The same N-body methodology and the latest ephemerides are used to compute a new orbital solution: a=1.6247 AU, e=0.5318, i=3.9750 degrees, Omega=326.4607 degrees and omega=109.7012 degrees. This new solution --which has an impact probability > 0.99999 and uncertainties in time and space of 0.2 s and 6 km, respectively-- is utilized to explore the past orbital evolution of the impactor as well as the presence of near-Earth objects moving in similar paths. A dynamical link between asteroid 2011 EO40 and the Chelyabinsk impactor is confirmed. Alternative orbital solutions are extensively explored.

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9 citations

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

...The largest predicted Yarkovsky drift rates are ∼10−7 AU yr−1 (see, e.g., Farnocchia et al. 2013), but the gravitationally induced changes in the values of the semimajor axes of 2003 BR47, 2011 EO40, and the virtual body associated with the solution displayed in Tables 1 and 2 are several orders of…...
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Journal Article•DOI•

Evolution of an Asteroid Family under YORP, Yarkovsky, and Collisions

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Francesco Marzari¹, Alessandro Rossi², Oleksiy Golubov³, Daniel J. Scheeres⁴•Institutions (4)

University of Padua¹, International Federation of Accountants², University of Kharkiv³, University of Colorado Boulder⁴

21 Aug 2020-The Astronomical Journal

TL;DR: In this article, a statistical code was developed to model the time evolution of the semi-major axis of an asteroid under YORP-Yarkovsky coupling, including the contributions of collisions.

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Abstract: Any population of asteroids, like asteroid families, will disperse in semi-major axis due to the Yarkovsky effect. The amount of drift is modulated by the asteroid spin state evolution which determines the balance between the diurnal and seasonal Yarkovsky force. The asteroid's spin state is, in turn, controlled in part by the YORP effect. The otherwise smooth evolution of an asteroid can be abruptly altered by collisions, which can cause impulsive changes in the spin state and can move the asteroid onto a different YORP track. In addition, collisions may also alter the YORP parameters by changing the superficial features and overall shape of the asteroid. Thus, the coupling between YORP and Yarkovsky is also strongly affected by the impact history of each body. To investigate this coupling we developed a statistical code modeling the time evolution of semi--major axis under YORP-Yarkovsky coupling. It includes the contributions of NYORP (normal YORP), TYORP (tangential YORP) and collisions whose effects are deterministically calculated and not added in a statistical way. We find that both collisions and TYORP increase the dispersion of a family in semi-major axis by making the spin axis evolution less smooth and regular. We show that the evolution of a family's structure with time is complex and collisions randomize the YORP evolution. In our test families we do not observe the formation of a 'YORP-eye' in the semi-major axis vs. diameter distribution, even after a long period of time. If present, the 'YORP-eye' might be a relic of an initial ejection velocity pattern of the collisional fragments.

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8 citations

Journal Article•DOI•

An ESA NEOCC Effort to Eliminate High Palermo Scale Virtual Impactors

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Marco Micheli¹, Detlef Koschny², Gerhard Drolshagen², Olivier Hainaut³, Fabrizio Bernardi - Show less +1 more•Institutions (3)

Serco Group¹, European Space Research and Technology Centre², European Southern Observatory³

06 Aug 2014-Earth Moon and Planets

TL;DR: In this paper, the initial results of a targeted effort of the ESA NEO Coordination Centre to obtain additional observational data in order to eliminate or reduce the impact probability estimate of a subset of the known near-Earth objects representing the highest fraction of the total known impact risk, as measured by the Palermo Scale.

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Abstract: In this work we summarize the initial results of a targeted effort of the ESA NEO Coordination Centre to obtain additional observational data in order to eliminate or reduce the impact probability estimate of a subset of the known near-Earth objects representing the highest fraction of the total known impact risk, as measured by the Palermo Scale.

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8 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).

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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....
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...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

[...]

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