Exogenic Dynamics, Cratering, and Surface Ages

Ivanov, B. A.; Hartmann, W. K.

doi:10.1016/b978-0-444-53802-4.00170-6

Cited by 35 publications

(47 citation statements)

References 258 publications

(353 reference statements)

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“…The traditional calibrated lunar chronology is based on the lunar production function of Neukum (1983), who computes N 1 /N 20 =995. For Mars Ivanov (2001) and Werner and Ivanov (2015) compute N 1 /N 20 = 419; this value was also used by Werner et al (2014). Note that these two scaling factors are both much lower than the value of 1400 used by Morbidelli et al (2012).…”

Section: The Moonmentioning

confidence: 99%

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

Brasser

Werner

Mojzsis

2020

Icarus

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Subsequent to the Moon's formation, late accretion to the terrestrial planets strongly modified the physical and chemical nature of their silicate crusts and mantles. Here, we combine dynamical N-body and Monte Carlo simulations to determine impact probabilities, impact velocities, and expected mass augmentation onto the terrestrial planets from three sources: planetesimals left over from primary accretion, asteroids from the hypothetical E-belt, and comets arriving from the outer Solar System. We present new estimates of the amount of cometary material striking the terrestrial planets in an early (ca. 4480 Ma) episode of planetesimal-driven giant planet migration . We conclude that the Moon and Mars suffer proportionally higher cometary accretion than Venus and Earth. We further conclude that the background mass addition from small leftover planetesimals to Earth and Mars is far less than independent estimates based on their respective mantle abundances of highly-siderophile elements and terrestrial tungsten isotopes. This supports the theory that both planets were struck by single large bodies that delivered most of their terminal mass augmentation since primary accretion, rather than a throng of smaller impactors. Our calculated lunar, martian and mercurian chronologies use the impacts recorded onto the planets from dynamical simulations rather than relying on the decline of the population as a whole. We present fits to the impact chronologies valid from 4500 Ma to ca. 3700 Ma by which time the low number of planetesimals remaining in the dynamical simulations causes the impact rate to drop artificially. The lunar timeline obtained from these dynamical simulations using nominal values for the masses of each contributing reservoir is at odds with both the calibrated Neukum (Neukum et al., 2001) and Werner (Werner et al., 2014; chronologies. For Mars, the match with its calibrated Werner chronology is no better; by increasing the mass of the E-belt by a factor of four the dynamical lunar and martian chronologies are in line with that of Werner (2019) and match constraints from the current population of Hungaria asteroids. Yet, neither of our dynamical timelines fit well with that of Neukum. The dynamical lunar and martian chronologies are also different from each other. Consequently, the usual extrapolation of such chronologies from one planetary body to the other is technically inappropriate.

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Section: The Moonmentioning

confidence: 99%

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

Brasser

Werner

Mojzsis

2020

Icarus

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“…(d) Strength-to-gravity transition diameter (D SG ) versus the cohesion in iSALE (Y 0 , lower x axis) and the effective strength (Y EFF , upper x axis) for targets with f = 0.6, 0.8, Φ = 20, 10%, and varying cohesions Y 0 . Note that the relation fromWerner and Ivanov [2015] is derived from numerical experiments conducted inWünnemann et al [2011] for a nonporous target with f = 0.8 and varying cohesions.Journal of Geophysical Research: Planets10.1002/2017JE005283 6. Incorporating the Effects of Coefficient of Friction and Porosity in the π Group Scaling Law…”

mentioning

confidence: 99%

The effect of target properties on transient crater scaling for simple craters

et al. 2017

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The effects of the coefficient of friction and porosity on impact cratering are not sufficiently considered in scaling laws that predict the crater size from a known impactor size, velocity, and mass. We carried out a systematic numerical study employing more than 1000 two‐dimensional models of simple crater formation under lunar conditions in targets with varying properties. A simple numerical setup is used where targets are approximated as granular or brecciated materials, and any compression of porous materials results in permanent compaction. The results are found to be consistent with impact laboratory experiments for water, low‐strength and low‐porosity materials (e.g., wet sand), and sands. Using this assumption, we found that both the friction coefficient and porosity are important for estimating transient crater diameters as is the strength term in crater scaling laws, i.e., the effective strength. The effects of porosity and friction coefficient on impact cratering were parameterized and incorporated into π group scaling laws, and predict transient crater diameters within an accuracy of ±5% for targets with friction coefficients f ≥ 0.4 and porosities Φ = 0–30%. Moreover, 90 crater scaling relationships are made available and can be used to estimate transient crater diameters on various terrains and geological units with different coefficient of friction, porosity, and cohesion. The derived relationships are most robust for targets with Φ > 10–15%, applicable for a lunar environment, and could therefore yield significant insights into the influence of target properties on cratering statistics.

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“…The size-frequency distribution of craters provides a way to date the planet's surface (e.g. Werner and Ivanov, 2015) and to estimate its erosive, volcanic (resurfacing) and interior activity.…”

Section: Consequences Of Impacts On the Interior Of Planetsmentioning

confidence: 99%

Geoscience for Understanding Habitability in the Solar System and Beyond

et al. 2019

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This paper reviews habitability conditions for a terrestrial planet from the point of view of geosciences. It addresses how interactions between the interior of a planet or a moon and its atmosphere and surface (including hydrosphere and biosphere) can affect habitability of the celestial body. It does not consider in detail the role of the central star but focusses more on surface conditions capable of sustaining life. We deal with fundamental issues of planetary habitability, i.e. the environmental conditions capable of sustaining life, and the above-mentioned interactions can affect the habitability of the celestial body.We address some hotly debated questions including:-How do core and mantle affect the evolution and habitability of planets? -What are the consequences of mantle overturn on the evolution of the interior and atmosphere? -What is the role of the global carbon and water cycles? -What influence do comet and asteroid impacts exert on the evolution of the planet? -How does life interact with the evolution of the Earth's geosphere and atmosphere?-How can knowledge of the solar system geophysics and habitability be applied to exoplanets?In addition, we address the identification of preserved life tracers in the context of the interaction of life with planetary evolution.

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Exogenic Dynamics, Cratering, and Surface Ages

Cited by 35 publications

References 258 publications

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

The effect of target properties on transient crater scaling for simple craters

Geoscience for Understanding Habitability in the Solar System and Beyond

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Exogenic Dynamics, Cratering, and Surface Ages

Cited by 35 publications

References 258 publications

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

The effect of target properties on transient crater scaling for simple craters

Geoscience for Understanding Habitability in the Solar System and Beyond

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Product

Resources

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Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga