Yarkovsky Drift Detections for 247 Near-Earth Asteroids

Greenberg, Adam; Margot, Jean-Luc; Verma, Ashok Kumar; Taylor, Patrick A.; Hodge, Susan E.

doi:10.3847/1538-3881/ab62a3

Cited by 67 publications

(69 citation statements)

References 35 publications

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“…As of this writing, there are published A 2 values for 244 NEAs on the JPL Small-Body Database. Yarkovsky drift rate detections for an additional 149 NEAs have also been reported in Greenberg et al (2020). The largest reported diameters among these asteroids belong to the 6.25 km (3200) Phaethon and 5.4 km (4179) Toutatis.…”

Section: Yarkovsky Follow-upmentioning

confidence: 74%

Thermal Properties of 1847 WISE-observed Asteroids

Hung¹,

Hanuš²,

Masiero³

et al. 2022

Planet. Sci. J.

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We present new thermophysical model fits of 1847 asteroids, deriving thermal inertia, diameter, and Bond and visible geometric albedo. We use thermal flux measurements obtained by the Wide-field Infrared Survey Explorer (WISE) during its fully cryogenic phase, when both the 12 μm (W3) and 22 μm (W4) bands were available. We take shape models and spin information from the Database of Asteroid Models from Inversion Techniques (DAMIT) and derive new shape models through lightcurve inversion and combining WISE photometry with existing DAMIT lightcurves. When we limit our sample to the asteroids with the most reliable shape models and thermal flux measurements, we find broadly consistent thermal inertia relations with recent studies. We apply fits to the diameters D (km) and thermal inertia Γ (J m−2 s−0.5 K−1) normalized to 1 au with a linear relation of the form log [ Γ ] = α + β log [ D ] , where we find α = 2.667 ± 0.059 and β = −0.467 ± 0.044 for our sample alone and α = 2.509 ± 0.017 and β = −0.352 ± 0.012 when combined with other literature estimates. We find little evidence of any correlation between rotation period and thermal inertia, owing to the small number of slow rotators to consider in our sample. While the large uncertainties on the majority of our derived thermal inertia only allow us to identify broad trends between thermal inertia and other physical parameters, we can expect a significant increase in high-quality thermal flux measurements and asteroid shape models with upcoming infrared and wide-field surveys, enabling even more thermophysical modeling of higher precision in the future.

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Section: Yarkovsky Follow-upmentioning

confidence: 74%

Thermal Properties of 1847 WISE-observed Asteroids

Hung¹,

Hanuš²,

Masiero³

et al. 2022

Planet. Sci. J.

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“…Using both models simultaneously ( 1 , 2 , 3 , and a Δv), we can determine the upper limit on these parameters to be 10 −11 , 10 −13 , and 10 −11 au/ 2 , and 10 −6 km/s respectively. These upper limits are 100 to 10,000 time smaller than usual values found for comets (Królikowska 2020) but 10 to 100 time higher than the typical values for the Yarkovsky effect for Near Earth object (Greenberg et al 2020). Excluding data prior to 2016, 2012, 2008, 2004, and 2000 also resulted in a non-detection of non-gravitational accelerations.…”

Section: Non-gravitational Accelerationmentioning

confidence: 56%

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

Devogèle

Ferrais

Jehin

et al. 2021

Monthly Notices of the Royal Astronomical Society

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In 2018 December, 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 h with a light-curve 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 (Yarkovsky–O’Keefe–Radzievskii–Paddack) 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 and 500 $\rm {\mu }$m. 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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“…A small drift in semi major-axis can also be measurable thanks to accurate astrometry deriving, for example from radar measurements, but they remain rare. Since this study, various papers have identified NEAs with a measurable drift in semi-major axis using astrometry (Nugent et al 2012;Farnocchia et al 2013;Desmars 2015;Del Vigna et al 2018;Greenberg et al 2020). Thanks to better recent as-trometry, such a drift is now measurable with reliability for more than 200 objects.…”

Section: Nongravitational Accelerationmentioning

confidence: 99%

The NAROO digitization center

Robert

Desmars²,

Lainey³

et al. 2021

A&A

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The New Astrometric Reduction of Old Observations (NAROO) center can be found at the Paris Observatory in Meudon, and it is dedicated to the measurement of astrophotographic plates and the analysis of old observations. The NAROO digitizer consists of a granite-based Newport-Microcontrol open-frame air-bearing XY positioning table, a scientific sCMOS camera, and a telecentric optical system. The plate holder assembly is suited for mounting glass plates up to 350 mm squared. The machine positioning stability is better than 15 nm, and its repeatability is better than 40 nm. With real photographic plate data, we were able to produce measurements with an accuracy better than 65 nm. The renewed interest about photographic plates concerns the expansion of the database of transient objects evolving in time, since digitization now makes it possible to measure images with a high level of accuracy and to identify all the available objects. The information extracted from such materials can be of an astrometric, photometric, and spectroscopic nature, when not purely imaging, with consequences in planetology, near-Earth asteroid risk assessment, astrophysical phenomena, and general relativity, to mention but a few. Through our scientific program in the Gaia era, we detail examples of current and upcoming uses for the community. We invite researchers to use our facilities and digitize their collection by answering our call for proposals.

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Yarkovsky Drift Detections for 247 Near-Earth Asteroids

Cited by 67 publications

References 35 publications

Thermal Properties of 1847 WISE-observed Asteroids

Thermal Properties of 1847 WISE-observed Asteroids

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

The NAROO digitization center

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