The fossilized size distribution of the main asteroid belt

By William Bottke, Daniel D. Durdaa, David Nesvornýa, Robert Jedickeb, Alessandro Morbidellic, David Vokrouhlickýd, Hal Levisona. 2003

534 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/9162dcba07fd18648c594966b1f3b5a5864a32aa

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Citations in the corpus

The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, unknown): “These values can be compared to the empirical αc of small main belt asteroids, considered to be near steady state (Bottke et al. 2005): αc = 3.00 ± 0.05 for 5 <∼ D <∼ 40 km (Ivezić et al. 2001), αc = 2.55 for 4 <∼ D <∼ 27 km if assuming pV = 0.1 (Gladman et al. 2009), and αc = 2.34 ± 0.05 for 2 <∼…”
A sawtooth-like timeline for the first billion years of lunar bombardment (2012, background): “Both SFDs are assumed to be the same as the current SFD of the main belt, which is justified because the shape of the latter has probably only experienced minor modifications by collisional evolution over the last 4 Gy (Bottke et al., 2005; Strom et al., 2005).”
What are the real constraints on the existence and magnitude of the late heavy bombardment (2007, background): “It is plausible that collisional evolution proceeds rapidly enough to quasi-equilibrium so that the larger impactors, which could have deeply penetrated the lunar regolith, had an asteroid-beltlike size distribution from early in the Moon’s history, but that depends on how much more massive the init”
COMETARY ORIGIN OF THE ZODIACAL CLOUD AND CARBONACEOUS MICROMETEORITES. IMPLICATIONS FOR HOT DEBRIS DISKS (2009, background): “According to Wyatt et al. (2007), the asteroidal debris disk is expected to decay by orders of magnitude from the time of Jupiter’s formation, which marked the start of the fragmentationdominated regime in the asteroid belt (e.g., Bottke et al. 2005), to LHB.”
Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System (2009, methodology): “For simplicity, we adopt a single albedo, qv 1⁄4 0:09, which is approximately representative over the size range of objects considered here (Bottke et al., 2005).”
A new method to determine the grain size of planetary regolith (2012, methodology): “The smoothed step function r3(g) was chosen because of the appearance of the data, which suggest a rather steep decrease of the regolith grain size for bodies of ∼ 100 km in size (g =∼ 5 × 10−2 m s−2), close to the value above which asteroids are thought to be primordial (Bottke et al., 2005).”
Differentiated Planetesimals and the Parent Bodies of Chondrites (2013, background): “See Lauretta & McSween 2006, pp. 19–52 Weiss BP, Berdahl S, Elkins-Tanton LT, Stanley S, Lima EA, Carporzen L. 2008.”
The rate of small impacts on Earth (2006, methodology): “Brown et al. (2002) estimated the rate of these events at approximately one every 1000 years.”
Rubble Pile Asteroids (2018, background): “4; Bottke et al. 2005,2015; Morbidelli et al. 2009).”
Fragment properties at the catastrophic disruption threshold: The effect of the parent body’s internal structure (2009, background): “emains small. This might explain why, to ﬁrst order, collisional evolution models could get away with only a single scaling law to reproduce the main characteristics of the asteroid populations (e.g. Bottke et al. 2005), despite the wide variety of internal properties that they can have. However, by”
Yarkovsky/YORP chronology of asteroid families (2006, background): “The change in slope is an artifact of comminution (Bottke et al., 2005b) and observational bias; it is found in all the families discussed in this paper.”
Size-frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families (2007, methodology): “According to modeling results, these steep SFDs eventually erode back to the same shape of the background main-belt SFD (Bottke et al., 2005c).”
A NEW CHRONOLOGY FOR THE MOON AND MERCURY (2008, methodology): “16 of Bottke et al. 2005b).”
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, background): “Once formed, the parent body would have experienced early thermal evolution by the decay of radiogenic nuclides (e.g., McSween et al., 2002), while its surface would have been battered by impacts for billions of years of cratering events (e.g., Bottke et al., 2005a,b).”
FORMATION OF KUIPER BELT BINARIES BY GRAVITATIONAL COLLAPSE (2010, background): “Since, according to Bottke et al. (2005), there are Ni ∼ 104 asteroids with ri > 5 km in the present asteroid belt, we can estimate that the present rate of unbinding collisions would be ∼ 2PiNiR21 = 2 × 10−10 yr−1, where Pi = 2.8 × 10−18 km−2 yr−1 is the intrinsic collision probability (see, e.g.,…”