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•

Cascade disruptions in asteroid clusters

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P. Fatka¹, P. Fatka², Petr Pravec¹, David Vokrouhlický²•Institutions (2)

Academy of Sciences of the Czech Republic¹, Charles University in Prague²

01 Mar 2020-Icarus

TL;DR: In this paper, the authors studied asteroid clusters suggesting a possibility of at least two disruption events in their recent history ( ≤ 5 Myr) and found four asteroid clusters, namely the clusters of (11842) Kap'bos, (14627) Emilkowalski, (63440) 2001 MD30 and (157123) 2004 NW5 that show at least 2 secondary separation events that occurred at significantly different times.

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7 citations

Journal Article•DOI•

(6478) Gault: Physical characterization of an active main-belt asteroid

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Maxime Devogele¹, Marin Ferrais², Emmanuel Jehin³, Nicholas Moskovitz⁴, Brian Skiff⁴, Stephen E. Levine⁴, Stephen E. Levine⁵, Annika Gustafsson⁶, Davide Farnocchia⁷, Marco Micheli, Colin Snodgrass⁸, Galin Borisov⁹, Galin Borisov¹⁰, Jean Manfroid³, Youssef Moulane¹¹, Youssef Moulane³, Youssef Moulane¹², Zouhair Benkhaldoun¹¹, A. Burdanov⁵, Francisco J. Pozuelos³, Michaël Gillon³, Julien de Wit⁵, Simon F. Green¹³, P. Bendjoya¹⁴, J. P. Rivet¹⁴, L. Abe¹⁴, David Vernet¹⁴, Colin Orion Chandler⁶, Chadwick A. Trujillo⁶ - Show less +25 more•Institutions (14)

University of Central Florida¹, Aix-Marseille University², University of Liège³, Lowell Observatory⁴, Massachusetts Institute of Technology⁵, Northern Arizona University⁶, California Institute of Technology⁷, University of Edinburgh⁸, Bulgarian Academy of Sciences⁹, Armagh Observatory¹⁰, Cadi Ayyad University¹¹, European Southern Observatory¹², Open University¹³, Centre national de la recherche scientifique¹⁴

07 Jun 2021-Monthly Notices of the Royal Astronomical Society

TL;DR: In this article, photometric and spectroscopic observations of the main-belt asteroid (6478 Gault) were conducted over two apparitions to monitor its activity, rotation period, composition, and possible non-gravitational orbital evolution.

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Abstract: In December 2018, the main-belt asteroid (6478) Gault was reported to display activity. Gault is an asteroid belonging to the Phocaea dynamical family and was not previously known to be active, nor was any other member of the Phocaea family. In this work we present the results of photometric and spectroscopic observations that commenced soon after the discovery of activity. We obtained observations over two apparitions to monitor its activity, rotation period, composition, and possible non-gravitational orbital evolution. We find that Gault has a rotation period of P = 2.4929 ± 0.0003 hours with a lightcurve amplitude of 0.06 magnitude. This short rotation period close to the spin barrier limit is consistent with Gault having a density no smaller than ρ = 1.85 g cm−3 and its activity being triggered by the YORP spin-up mechanism. Analysis of the Gault phase curve over phase angles ranging from 0.4○ to 23.6○ provides an absolute magnitude of H = 14.81 ± 0.04, G1 = 0.25 ± 0.07, and G2 = 0.38 ± 0.04. Model fits to the phase curve find the surface regolith grain size constrained between 100-500 μm. Using relations between the phase curve and albedo we determine that the geometrical albedo of Gault is pv = 0.26 ± 0.05 corresponding to an equivalent diameter of D=2.8+0.4−0.2 km. Our spectroscopic observations are all consistent with an ordinary chondrite-like composition (S, or Q-type in the Bus-DeMeo taxonomic classification). A search through archival photographic plate surveys found previously unidentified detections of Gault dating back to 1957 and 1958. Only the latter had been digitized, which we measured to nearly double the observation arc of Gault. Finally, we did not find any signal of activity during the 2020 apparition or non-gravitational effects on its orbit.

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7 citations

Journal Article•DOI•

Low thermal conductivity of the superfast rotator (499998) 2011 PT

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Marco Fenucci¹, Bojan Novaković¹, David Vokrouhlický², Robert Weryk³•Institutions (3)

University of Belgrade¹, Charles University in Prague², University of Hawaii³

01 Mar 2021-Astronomy and Astrophysics

TL;DR: In this article, a model for constraining the thermal conductivity of the surface of the small, fast-rotating near-Earth asteroids was developed based on the comparison of the measured Yarkovsky drift and a predicted value using a theoretical model that depends on the orbital, physical and thermal parameters of the object.

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Abstract: Context. Asteroids with a diameter of up to a few dozen meters may spin very fast and complete an entire rotation within a few minutes. These small and fast-rotating bodies are thought to be monolithic objects because the gravitational force due to their small size is not strong enough to counteract the strong centripetal force caused by the fast rotation. This argument means that the rubble-pile structure is not feasible for these objects. Additionally, it is not clear whether the fast spin prevents dust and small particles (regolith) from being kept on their surface.Aims. We develop a model for constraining the thermal conductivity of the surface of the small, fast-rotating near-Earth asteroids. This model may suggest whether regolith is likely present on these objects.Methods. Our approach is based on the comparison of the measured Yarkovsky drift and a predicted value using a theoretical model that depends on the orbital, physical and thermal parameters of the object. The necessary parameters are either deduced from statistical distribution derived for near-Earth asteroids population or determined from observations with associated uncertainty. With this information, we performed Monte Carlo simulations and produced a probability density distribution for the thermal conductivity.Results. Applying our model to the superfast rotator asteroid (499998) 2011 PT, we find that the measured Yarkovsky drift can only be achieved when the thermal conductivity K of the surface is low. The resulting probability density function for the conductivity is bimodal, with two most likely values being around 0.0001 and 0.005 W m−1 K−1 . Based on this, we find that the probability that K is lower than 0.1 W m−1 K−1 is at least 95%. This low thermal conductivity might indicate that the surface of 2011 PT is covered with a thermal insulating layer, composed of a regolith-like material similar to lunar dust.

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7 citations

Journal Article•DOI•

Low thermal conductivity of the superfast rotator (499998) 2011 PT

[...]

Marco Fenucci¹, Bojan Novaković¹, David Vokrouhlický², Robert Weryk³•Institutions (3)

University of Belgrade¹, Charles University in Prague², University of Hawaii³

12 Jan 2021-arXiv: Earth and Planetary Astrophysics

TL;DR: In this paper, a model for constraining the thermal conductivity of the surface of the small, fast-rotating near-Earth asteroids was developed based on the comparison of the measured Yarkovsky drift and a predicted value using a theoretical model that depends on the orbital, physical and thermal parameters of the object.

...read moreread less

Abstract: Context: Asteroids with a diameter of up to a few dozen meters may spin very fast and complete an entire rotation within a few minutes. These small and fast-rotating bodies are thought to be monolithic objects because the gravitational force due to their small size is not strong enough to counteract the strong centripetal force caused by the fast rotation. Additionally, it is not clear whether the fast spin prevents dust and small particles (regolith) from being kept on their surface. Aims: We develop a model for constraining the thermal conductivity of the surface of the small, fast-rotating near-Earth asteroids. This model may suggest whether regolith is likely present on these objects. Methods: Our approach is based on the comparison of the measured Yarkovsky drift and a predicted value using a theoretical model that depends on the orbital, physical and thermal parameters of the object. The necessary parameters are either deduced from statistical distribution derived for near-Earth asteroids population or determined from observations with associated uncertainty. With this information, we performed Monte Carlo simulations and produced a probability density distribution for the thermal conductivity. Results: Applying our model to the superfast rotator asteroid (499998) 2011 PT, we find that the measured Yarkovsky drift can only be achieved when the thermal conductivity $K$ of the surface is low. The resulting probability density function for the conductivity is bimodal, with two most likely values being around 0.0001 and 0.005 W m$^{-1}$ K$^{-1}$. Based on this, we find that the probability that $K$ is lower than 0.1 W m$^{-1}$ K$^{-1}$ is at least 95\%. This low thermal conductivity might indicate that the surface of 2011 PT is covered with a thermal insulating layer, composed of a regolith-like material similar to lunar dust.

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6 citations

Journal Article•DOI•

Spin Change of Asteroid 2012 TC4 Probably by Radiation Torques

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Hee-Jae Lee¹, Hee-Jae Lee², Josef Ďurech³, David Vokrouhlický³, P. Pravec⁴, Hong-Kyu Moon¹, William Ryan⁵, Myung-Jin Kim¹, Chun-Hwey Kim², Young-Jun Choi¹, Young-Jun Choi⁶, Paolo Bacci, Joe Pollock⁷, Rolf Apitzsch - Show less +10 more•Institutions (7)

Korea Astronomy and Space Science Institute¹, Chungbuk National University², Charles University in Prague³, Academy of Sciences of the Czech Republic⁴, New Mexico Institute of Mining and Technology⁵, Korea University of Science and Technology⁶, Appalachian State University⁷

11 Feb 2021-The Astronomical Journal

TL;DR: Asteroid 2012 TC4 is a small near-Earth object that was observed during its Earth close-approaches in 2012 and 2017 as discussed by the authors, and its rotation and precession periods are significantly different for these two data sets and they must have changed between or during the two apparitions.

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Abstract: Asteroid 2012 TC4 is a small ($\sim$10 m) near-Earth object that was observed during its Earth close approaches in 2012 and 2017. Earlier analyses of light curves revealed its excited rotation state. We collected all available photometric data from the two apparitions to reconstruct its rotation state and convex shape model. We show that light curves from 2012 and 2017 cannot be fitted with a single set of model parameters -- the rotation and precession periods are significantly different for these two data sets and they must have changed between or during the two apparitions. Nevertheless, we could fit all light curves with a dynamically self-consistent model assuming that the spin states of 2012 TC4 in 2012 and 2017 were different. To interpret our results, we developed a numerical model of its spin evolution in which we included two potentially relevant perturbations: (i) gravitational torque due to the Sun and Earth, and (ii) radiation torque known as the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. Despite our model simplicity, we found that the role of gravitational torques is negligible. Instead, we argue that the observed change of its spin state may be plausibly explained as a result of the YORP torque. To strengthen this interpretation we verify that (i) the internal energy dissipation due to material inelasticity, and (ii) an impact with a sufficiently large interplanetary particle are both highly unlikely causes its observed spin state change. If true, this is the first case when the YORP effect has been detected for a tumbling body.

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6 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

[...]

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....
[...]

Journal Article•DOI•

THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics

[...]

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)....
[...]

Application of photometric models to asteroids.

[...]

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