The Time-Dependent Intense Bombardment of the Primordial Earth/Moon System

By W. Hartmann, G. Ryder, L. Dones, D. Grinspoon. 2000

209 citations recorded by the source corpus.

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Citations in the corpus

Back to the Moon: The scientific rationale for resuming lunar surface exploration (2012, background): “…uncertainty over whether the lunar cratering rate has declined monotonically since the formation of the Moon, or whether there was a bombardment ‘cataclysm’ between about 3.8 and 4.0 billion years ago characterised by an unusually high rate of impacts (Hartmann et al., 2000; Stöffler et al., 2006).”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “The second is that they wanted to avoid locking th selves into a dynamical evolution scenario that would lik become obsolete as planet formation models increase sophistication (e.g., next generation models will likely clude the effects of dynamical friction between planet embryos and planetesimals, ”
COMETARY ORIGIN OF THE ZODIACAL CLOUD AND CARBONACEOUS MICROMETEORITES. IMPLICATIONS FOR HOT DEBRIS DISKS (2009, background): “For comparison, the mass of large impactors estimated from the number and size distribution of lunar basins is 6 × 10(21) g (Hartmann et al., 2000).”
Cratering History and Lunar Chronology (2006, methodology): “…craters in the diameter bin DLFT < D < DRGT, where DLFT and DRGT are the left and right bin boundary and the standard bin width is DRGT= 21/2DLFT. Hartmann et al. (2000) approximated the tabulated HPF in the form of a piece-wise, three-segment power law (coefficients first published jointly by…”
What are the real constraints on the existence and magnitude of the late heavy bombardment (2007, background): “Hartmann (2003) has tried to rebut his presumed co-author’s criticism (in Hartmann et al., 2000) by arguing that impact melts produced by early basins would, indeed, have been subsequently “destroyed” (specifically by being pulverized by later large-crater-forming impacts to particle sizes 60 µm,…”
Origins of volatile elements (H, C, N, noble gases) on Earth and Mars in light of recent results from the ROSETTA cometary mission (2016, unknown): “2 × 1023 g (Hartmann et al., 2002) down to 4 × 1022 g (assuming that the TLHB started at the time of formation of Nectaris basin; Morbidelli et al.”
Nonuniform cratering of the Moon and a revised crater chronology of the inner Solar System (2011, background): “…of20 times more numerous than today, possibly due to the massive injection in the21 inner system of main-belt and/or Kuiper-belt objects about 700 Ma after the22 Moon formed, an event known as the Late Heavy Bombardment (LHB) (see23 Gomes et al., 2005; Tera et al., 1974; Hartmann et al., 2000).”
Bias-corrected population, size distribution, and impact hazard for the near-Earth objects (2004, background): “A primary difference between the crater production fu tion of Neukum et al. and that of BVTP is the inclusion craters from the older lunar highlands which may have b subjected to a substantially higher cratering rate during Late Heavy Bombardment(Hartmann et al., 2000).”
The faint young Sun problem (2012, background): “…of the Late Heavy Bombardment (∼ 4.0 to 3.8 Ga) already before the beginning of the Archean [Tera et al., 1974; Wetherill , 1975; Sleep et al., 1989; Hartmann et al., 2000; Kring and Cohen, 2002], and was at most one order of magnitude higher than today after the Late Heavy Bombardment, too low…”
The fossilized size distribution of the main asteroid belt (2003, background): “…above, we lieve the most plausible solution to this enigma is that same dynamical instability that produced the Late He Bombardment∼3.9 Gyr ago (e.g.,Hartmann et al., 2000 Levison et al., 2001) also scrambled our ability to compu useful proper(a, e, i) elements beyond this epoch; in effe this…”
The timeline of the lunar bombardment: Revisited (2018, background): “oon experienced a heavy bombardment about 600 My after planet formation during which the youngest lunar basins, like Imbrium and Orientale (and possibly also Serenitatis) formed (for reviews see e.g. Hartmann et al., 2000; Chapman et al., 2007; Norman, 2009). We call this period of intense bombardme”
Early life on land and the first terrestrial ecosystems (2013, background): “It is plausible then, that by the end of the heavy bombardment (Gomes et al. 2005; Hartmann et al. 2000) some ~3,800 Ma ago, the primitive lands and oceans were open niches ready for the pioneering and rapidly evolving microscopic life forms, for which occasional “sterilizing” perturbations may be…”
Cataclysmic bombardment throughout the inner solar system 3.9–4.0 Ga (2002, background): “[17] Depending on the size distribution among impactors, the Earth is hit by 13–500 times more mass than the Moon [Zahnle and Sleep, 1997; Hartmann et al., 2000], implying 8.7 1022 to 4.4 1024 g, with a median of 3 1023 g, hit the Earth during the bombardment.”