Water delivery to the Moon by asteroidal and cometary impacts

Svetsov, V. V.; Шувалов, В. В.

doi:10.1016/j.pss.2015.09.011

Cited by 45 publications

(32 citation statements)

References 45 publications

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“…Survivability of such projectile fragments to the Moon's surface may be possible at these collisional velocities and associated peak shock pressure regimes. However, preservation of impactor material will be facilitated further by relatively low (\4 km/s) impact velocities (Crawford et al 2008;Armstrong 2011), by oblique (\10 degrees) impact angles where material can be spalled off the projectile during impact (Pierazzo and Melosh 2000; Bland et al 2008;Svetsov and Shuvalov 2015;Schultz and Crawford 2016), and by incorporation of impactor material into central peaks formed during the crater formation process (Yue et al 2013). Recent laboratory experiments have also shown that the material properties, specifically porosity, of the impactor target material further helps to b Large FeNi metal assemblages found in a crystalline (plagioclase, pyroxene) impact melt breccia clast extracted from regolith breccia 60016.…”

Section: Asteroidsmentioning

confidence: 99%

“…However, recent hydrocode modelling work by Svetsov and Shuvalov (2015) suggests that whilst 99 % of all water is vaporised in cometary impacts, a small portion of hydrated minerals can survive the impact event and *1.5 % of all lunar craters could potentially contain this hydrated mineral debris. A larger fraction of comet impactors are lost from the Moon than asteroids, because they hit at higher velocities.…”

Section: Cometary Impactorsmentioning

confidence: 99%

“…Locating and characterising volatile-rich or organic-phase debris sourced from comets or primitive asteroids (Svetsov and Shuvalov 2015) will require using non-destructive methods like RAMAN or FTIR spectroscopy that fingerprint organic molecules or phyllosilicates (Fries and Steele 2007) or thermally-altered remnants of such material, which have a characteristic texture and mineralogy (Zolensky et al 2008;Burchell et al 2014a). …”

Section: Volatile-rich Materials From Primitive Asteroids and Cometsmentioning

confidence: 99%

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The Moon: An Archive of Small Body Migration in the Solar System

et al. 2016

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The Moon is an archive of impact cratering in the Solar System throughout the past 4.5 billion years. It preserves this record better than larger, more complex planets like the Earth, Mars and Venus, which have largely lost their ancient crusts through geological reprocessing and hydrospheric/atmospheric weathering. Identifying the parent bodies of impactors (i.e. asteroid bodies, comets from the Kuiper belt or the Oort Cloud) provides geochemical and chronological constraints for models of Solar System dynamics, helping to better inform our wider understanding of the evolution of the Solar System and the transfer of small bodies between planets. In this review article, we discuss the evidence for populations of impactors delivered to the Moon at different times in the past. We also propose approaches to the identification and characterisation of meteoritic material on the Moon in the context of future lunar exploration efforts.

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Section: Asteroidsmentioning

confidence: 99%

Section: Cometary Impactorsmentioning

confidence: 99%

Section: Volatile-rich Materials From Primitive Asteroids and Cometsmentioning

confidence: 99%

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The Moon: An Archive of Small Body Migration in the Solar System

et al. 2016

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“…The preservation of impactor substance at asteroid and cometary impacts has been investigated in Svetsov and Shuvalov (2015). According to their estimations at the impact angle of 45°almost 50 % of impactor mass (for ordinary chondrite) remains in the crater at impact velocity B12 km/s and almost 90 % at impact velocity B9 km/s.…”

Section: Preservation Of Impactor Substance In the Crater After Its Fmentioning

confidence: 99%

“…Only one stony-iron impactor have 12 km/s. We calculated the impactor mass inside the crater Shackleton using models from Bland et al (2008) for all types of impactors, excluding comets, and model from Svetsov and Shuvalov (2015) for ordinary and carbonaceous chondrites and comets (Table 4). We obtained that according to conclusions in the paper by Bland et al (2008), since the present study estimated the possible impact angle at C45°and the velocity at B6 km/s, more than 50 % of the impactor mass could be present inside the crater.…”

Section: Shackleton Crater Characteristicsmentioning

confidence: 99%

On the Nature of the Impactor That Formed the Shackleton Crater on the Moon

Pugacheva¹,

Феоктистова²,

Шевченко³

2016

Earth Moon Planets

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The present paper attempts to assess the characteristics of the impactor that formed the Shackleton crater, located at the south pole of the Moon. The crater's morphometric parameters were analyzed based on the data of the Lunar Orbiter Laser Altimeter aboard the Lunar Reconnaissance Orbiter. Conclusions were drawn regarding the possible range of the impact angle and the parameters of the transient crater, such as depth and volume. The thickness of ejecta deposits on the transient crater rim and the volume of these deposits at a certain distance from the crater rim were assessed. These assessments enabled determining the type and characteristics of impactors (velocity, density, size, and impact angle) that could have formed the Shackleton crater. It was shown that the Shackleton crater could have been formed by an impact of a low-velocity (3 km/s) comets with diameter 4-4.5 km, chondrite or achondrite with a diameter of 2 km at a 45°-50°angle, whose velocity did not exceed 6 km/s, as well as stony-iron or iron-nickel impactors with a 1-2 km diameter for stony-iron asteroids and 1-1.5 km for iron-nickel asteroids. The impact velocity of stony-iron impactors, according to the authors' calculations, can reach 12 km/s. The impact velocities of iron-nickel asteroids range from 6 to 9 km/s. The impactor's substance mass that could have remained in the crater after it was formed was assessed.

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Effect of impact velocity and acoustic fluidization on the simple‐to‐complex transition of lunar craters

et al. 2017

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We use numerical modeling to investigate the combined effects of impact velocity and acoustic fluidization on lunar craters in the simple‐to‐complex transition regime. To investigate the full scope of the problem, we employed the two widely adopted Block‐Model of acoustic fluidization scaling assumptions (scaling block size by impactor size and scaling by coupling parameter) and compared their outcomes. Impactor size and velocity were varied, such that large/slow and small/fast impactors would produce craters of the same diameter within a suite of simulations, ranging in diameter from 10 to 26 km, which straddles the simple‐to‐complex crater transition on the Moon. Our study suggests that the transition from simple to complex structures is highly sensitive to the choice of the time decay and viscosity constants in the Block‐Model of acoustic fluidization. Moreover, the combination of impactor size and velocity plays a greater role than previously thought in the morphology of craters in the simple‐to‐complex size range. We propose that scaling of block size by impactor size is an appropriate choice for modeling simple‐to‐complex craters on planetary surfaces, including both varying and constant impact velocities, as the modeling results are more consistent with the observed morphology of lunar craters. This scaling suggests that the simple‐to‐complex transition occurs at a larger crater size, if higher impact velocities are considered, and is consistent with the observation that the simple‐to‐complex transition occurs at larger sizes on Mercury than Mars.

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Water delivery to the Moon by asteroidal and cometary impacts

Cited by 45 publications

References 45 publications

The Moon: An Archive of Small Body Migration in the Solar System

The Moon: An Archive of Small Body Migration in the Solar System

On the Nature of the Impactor That Formed the Shackleton Crater on the Moon

Effect of impact velocity and acoustic fluidization on the simple‐to‐complex transition of lunar craters

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