Numerical predictions of surface effects during the 2029 close approach of Asteroid 99942 Apophis

Yu, Yang; Richardson, D. C.; Michel, Patrick; Schwartz, S. R.; Ballouz, Ronald-Louis

doi:10.1016/j.icarus.2014.07.027

Cited by 81 publications

(75 citation statements)

References 25 publications

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“…Recent work featuring a higher level of sophistication in the modelling of tidal disruption (e.g. Movshovitz et al 2012;Yu et al 2014) showcases potential future directions for follow-up studies. In these cases, particles are idealized not as indestructible hard spheres, but rather as soft spheres (Schwartz, Richardson & Michel 2012).…”

Section: Simulation Detailsmentioning

confidence: 99%

Formation of planetary debris discs around white dwarfs – I. Tidal disruption of an extremely eccentric asteroid

Veras

Leinhardt

Bonsor

et al. 2014

Monthly Notices of the Royal Astronomical Society

198

247

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ABSTRACT25-50 per cent of all white dwarfs (WDs) host observable and dynamically active remnant planetary systems based on the presence of close-in circumstellar dust and gas and photospheric metal pollution. Currently accepted theoretical explanations for the origin of this matter include asteroids that survive the star's giant branch evolution at au-scale distances and are subsequently perturbed on to WD-grazing orbits following stellar mass-loss. In this work, we investigate the tidal disruption of these highly eccentric (e > 0.98) asteroids as they approach and tidally disrupt around the WD. We analytically compute the disruption time-scale and compare the result with fully self-consistent numerical simulations of rubble piles by using the N-body code PKDGRAV. We find that this time-scale is highly dependent on the orbit's pericentre and largely independent of its semimajor axis. We establish that spherical asteroids readily break up and form highly eccentric collisionless rings, which do not accrete on to the WD without additional forces such as radiation or sublimation. This finding highlights the critical importance of such forces in the physics of WD planetary systems.

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Section: Simulation Detailsmentioning

confidence: 99%

Formation of planetary debris discs around white dwarfs – I. Tidal disruption of an extremely eccentric asteroid

Veras

Leinhardt

Bonsor

et al. 2014

Monthly Notices of the Royal Astronomical Society

198

247

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“…Bennu's 4 equatorial peaks are still a puzzle. Perhaps a tidal excitation would better excite the football-shaped mode without exciting an l = 3 triangular mode, though a nearby encounter with a larger body would be required (e.g., see Press and Teukolsky 1977;Yu et al 2014;Quillen et al 2016a). Alternatively perhaps an excited l = 3 triangular mode would decay more quickly than the football-shaped mode letting the body surface slump at four rather than two equatorial peaks.…”

Section: Discussionmentioning

confidence: 99%

Impact excitation of a seismic pulse and vibrational normal modes on asteroid Bennu and associated slumping of regolith

Quillen

Zhao

Chen

et al. 2019

Icarus

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the equatorial ridge. We explore simple flow models for the morphology of vibration induced surface slumping. We find that the initial seismic pulse is unlikely to cause large shape changes. Long lasting seismic reverberation on Bennu caused by a near equatorial impact could have raised the height of its equatorial ridge by a few meters and raised two peaks on it, one near impact site and the other near its antipode.

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“…Its encounter with the gravity of the Earth-Moon system may have shed off substantial amounts of asteroid debris already at distances of 10,000-20,000 km from Earth. Asteroids entering within the Roche limit get affected by tidal gravity, and anything between loss of surface material to complete disruption of the asteroid may happen (Richardson et al, 1998;Nesvorný et al, 2010;Tóth et al, 2011;Schunova et al, 2014;Yu et al, 2014). Recent space missions to asteroids Itokawa and Eros (mean diameters 0.3 and 17 km, respectively) have shown that small to large asteroids have a significant layer of lose regolith or "rubble-pile" debris on their surface (Murdoch et al, 2013).…”

Section: Discussionmentioning

confidence: 99%

“…Recent space missions to asteroids Itokawa and Eros (mean diameters 0.3 and 17 km, respectively) have shown that small to large asteroids have a significant layer of lose regolith or "rubble-pile" debris on their surface (Murdoch et al, 2013). Model simulations show that regolith avalanches are expected on asteroids affected by Earth's gravity (Yu et al, 2014). There are a number of tidal effects that can disturb the surface of an asteroid during a planetary encounter, for example, the tidal torque may spin up an asteroid, and centrifugal forces exceeding the asteroids gravity may move the regolith (Nesvorný et al, 2010).…”

Section: Discussionmentioning

confidence: 99%

Fragments of Late Eocene Earth-impacting asteroids linked to disturbance of asteroid belt

Schmitz

Boschi

Cronholm

et al. 2015

Earth and Planetary Science Letters

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Available online xxxx Editor: B. Marty Keywords: Late Eocene Popigai crater helium-3 ordinary chondrite asteroid belt ice ageThe onset of Earth's present icehouse climate in the Late Eocene coincides with astronomical events of enigmatic causation. At ∼36 Ma ago the 90-100 km large Popigai and Chesapeake Bay impact structures formed within ∼10-20 ka. Enrichments of 3 He in coeval sediments also indicate high fluxes of interplanetary dust to Earth for ∼2 Ma. Additionally, several medium-sized impact structures are known from the Late Eocene. Here we report from sediments in Italy the presence of abundant ordinary chondritic chromite grains (63-250 μm) associated with the ejecta from the Popigai impactor. The grains occur in the ∼40 cm interval immediately above the ejecta layer. Element analyses show that grains in the lower half of this interval have an apparent H-chondritic composition, whereas grains in the upper half are of L-chondritic origin. The grains most likely originate from the regoliths of the Popigai and the Chesapeake Bay impactors, respectively. These asteroids may have approached Earth at comparatively low speeds, and regolith was shed off from their surfaces after they passed the Roche limit. The regolith grains then settled on Earth some 100 to 1000 yrs after the respective impacts. Further neon and oxygen isotopic analyses of the grains can be used to test this hypothesis. If the Popigai and Chesapeake Bay impactors represent two different types of asteroids one can rule out previous explanations of the Late Eocene extraterrestrial signatures invoking an asteroid shower from a single parent-body breakup. Instead a multi-type asteroid shower may have been triggered by changes of planetary orbital elements. This could have happened due to chaos-related transitions in motions of the inner planets or through the interplay of chaos between the outer and inner planets. Asteroids in a region of the asteroid belt where many ordinary chondritic bodies reside, were rapidly perturbed into orbital resonances. This led to an increase in small to medium-sized collisional breakup events over a 2-5 Ma period. This would explain the simultaneous delivery of excess dust and asteroids to the inner solar system. Independent evidence for our scenario are the common cosmic-ray exposure ages in the range of ca. 33-40 Ma for recently fallen H and L chondrites. The temporal coincidence of gravity disturbances in the asteroid belt with the termination of ice-free conditions on Earth after 250 Ma is compelling. We speculate that this coincidence and a general correlation during the past 2 Ga between K-Ar breakup ages of parent bodies of the ordinary chondrites and ice ages on Earth suggest that there may exist an astronomical process that disturbs both regions of the inner asteroid belt and Earth's orbit with a potential impact on Earth's climate.

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Numerical predictions of surface effects during the 2029 close approach of Asteroid 99942 Apophis

Cited by 81 publications

References 25 publications

Formation of planetary debris discs around white dwarfs – I. Tidal disruption of an extremely eccentric asteroid

Formation of planetary debris discs around white dwarfs – I. Tidal disruption of an extremely eccentric asteroid

Impact excitation of a seismic pulse and vibrational normal modes on asteroid Bennu and associated slumping of regolith

Fragments of Late Eocene Earth-impacting asteroids linked to disturbance of asteroid belt

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