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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Special Group of the Potentially Hazardous Asteroids

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Ireneusz Wlodarczyk

01 Feb 2020

TL;DR: In this article, a uniform selection and weighing method was used to compute the keplerian orbital elements for the epoch October 9, 2018 together with the new computed non-gravitational parameters A2.

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Abstract: Up to now, i.e. until March 15, 2019, there have been no uniform and up-todate computed orbits of so called Special asteroids: 29075 (1950DA), 99942 (Apophis), 101955 (Bennu) and 410777 (2009FD). In this work, based on all available astrometric and radar observations up to March 15, 2019, and a uniform selection and weighing method, I have computed keplerian orbital elements for the epoch October 9, 2018 together with the new computed non-gravitational parameters A2. Also, I have calculated the updated risk tables for these asteroids based on all observations, including non-gravitational parameter A2, the DE431 version of JPL’s planetary ephemerides and perturbation from 16 massive asteroids and the dwarf planet Pluto.

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3 citations

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

...Also, I used the DE431 version of JPL’s planetary ephemerides and additional 16 massive perturbing asteroids and dwarf planet Pluto as in Del Vigna et al. (2018), and in Farnocchia et al. (2013b)....
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...…(99942) Apophis computed using shorter observational arc and different Solar System models are widely published, e.g. in Vokrouhlicky et al.(2015), Farnocchia et al.(2013b), Bancelin et al.(2012), Zizka and Vokrouhlicy(2011), Krolikowska and Sitarski(2010), Krolikowska et al.(2009) and in…...
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Journal Article•DOI•

OUP accepted manuscript

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02 Feb 2022-Monthly Notices of the Royal Astronomical Society

TL;DR: In this article , a newly discovered pair of near-Earth objects (NEOs): 2019 PR2 and 2019 QR6) were studied based on broad-band photometry, and two models of comet-like non-gravitational forces based on water or CO sublimation were implemented.

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Abstract: ABSTRACT Asteroid pairs are genetically related asteroids that recently separated (<few million years), but still reside on similar heliocentric orbits. A few hundred of these systems have been identified, primarily in the asteroid main belt. Here, we studied a newly discovered pair of near-Earth objects (NEOs): 2019 PR2 and 2019 QR6. Based on broad-band photometry, we found these asteroids to be spectrally similar to D-types, a type rare amongst NEOs. We recovered astrometric observations for both asteroids from the Catalina Sky Survey from 2005, which significantly improved their fitted orbits. With these refinements we ran backwards orbital integrations to study formation and evolutionary history. We found that neither a pure gravitational model nor a model with the Yarkovsky effect could explain their current orbits. We thus implemented two models of comet-like non-gravitational forces based on water or CO sublimation. The first model assumed quasi-continuous, comet-like activity after separation, which suggested a formation time of the asteroid pair $300^{+120}_{-70}$ yr ago. The second model assumed short-term activity for up to one heliocentric orbit (∼13.9 yr) after separation, which suggested that the pair formed 272 ± 7 yr ago. Image stacks showed no activity for 2019 PR2 during its last perihelion passage. These results strongly argue for a common origin that makes these objects the youngest asteroid pair known to date. Questions remain regarding whether these objects derived from a parent comet or asteroid, and how activity may have evolved since their separation.

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3 citations

Journal Article•DOI•

A Novel Approach to Asteroid Impact Monitoring

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Javier Roa, Davide Farnocchia, Steven R. Chesley

01 Dec 2021-The Astronomical Journal

3 citations

Journal Article•DOI•

Discovery and dynamical characterization of the Amor-class asteroid 2012 XH16

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I. Wlodarczyk, K. Černis¹, R. P. Boyle², V. Laugalys¹•Institutions (2)

Vilnius University¹, Steward Health Care System²

01 Mar 2014-Monthly Notices of the Royal Astronomical Society

2 citations

Journal Article•DOI•

The Random Walk of Cars and Their Collision Probabilities with Planets

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Hanno Rein, Daniel Tamayo, David Vokrouhlický

23 May 2018

TL;DR: In this article, the authors performed N-body simulations to determine the fate of the Tesla Roadster over the next 15 Myr, and calculated a dynamical half-life of the vehicle with some 22, 12% and 12% of realizations impacting the Earth, Venus, and the Sun within one half life, respectively.

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Abstract: On 6 February 2018, SpaceX launched a Tesla Roadster on a Mars-crossing orbit. We perform N-body simulations to determine the fate of the object over the next 15 Myr. The orbital evolution is initially dominated by close encounters with the Earth. While a precise orbit can not be predicted beyond the next several centuries due to these repeated chaotic scatterings, one can reliably predict the long-term outcomes by statistically analyzing a large suite of possible trajectories with slightly perturbed initial conditions. Repeated gravitational scatterings with Earth lead to a random walk. Collisions with the Earth, Venus and the Sun represent primary sinks for the Roadster’s orbital evolution. Collisions with Mercury and Mars, or ejections from the Solar System by Jupiter, are highly unlikely. We calculate a dynamical half-life of the Tesla of approximately 15 Myr, with some 22%, 12% and 12% of Roadster orbit realizations impacting the Earth, Venus, and the Sun within one half-life, respectively. Because the eccentricities and inclinations in our ensemble increase over time due to mean-motion and secular resonances, the impact rates with the terrestrial planets decrease beyond a few million years, whereas the impact rate on the Sun remains roughly constant.

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2 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