The fossilized size distribution of the main asteroid belt

Bottke, W. F.; Durda, D. D.; Nesvorný, David; Jedicke, Robert; Morbidelli, Alessandro; Vokrouhlický, David; Levison, H. F.

doi:10.1016/j.icarus.2004.10.026

Cited by 535 publications

(704 citation statements)

References 124 publications

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“…However, rather sensationally, the same analysis also shows an internal consistency of the measurements that puts an upper limit of only about 4000 years on the interval of time over which the (asteroid) parent body of the analyzed samples formed. This provides direct evidence for a very rapid planetesimal formation mechanism, consistent with recent astrophysical ideas and empirical evidence (Johansen & Lacerda 2010;Bottke et al 2005;Morbidelli et al 2009). …”

Section: Evidence From Cosmo-chemistrysupporting

confidence: 86%

Formation of brown dwarfs and planets

Nordlund

2010

Proc. IAU

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Abstract. Brown dwarfs and massive planets have similar structures, and there is probably an overlap in mass between the most massive planets and the lowest mass brown dwarfs. This raises questions as to what extent the structures of the most massive planets and lowest mass brown dwarfs differ, and what similarities (or not) there might be between their formation mechanisms. Here I discuss these issues on the background of recent numerical simulations of star formation, new evidence from cosmochemistry about the conditions in the early solar system, and recently discovered mechanisms that can expedite planetesimal and possibly planet formation greatly.

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Section: Evidence From Cosmo-chemistrysupporting

confidence: 86%

Formation of brown dwarfs and planets

Nordlund

2010

Proc. IAU

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“…This calculation is complicated by the fact that any given debris particle will interact with particles with a range of sizes, with the outcomes of such collisions ranging from cratering to complete pulverisation. For this reason the collisional evolution of debris populations is often studied numerically (Thébault et al 2003;Krivov et al 2005;Bottke et al 2005). However, this is not necessary to understand what happens, because for most common assumptions about collisional outcomes, once the size distribution has reached steady state it tends to a shape that can be readily calculated (O'Brien and Greenberg 2003;Wyatt et al 2011).…”

Section: Collisional Evolutionmentioning

confidence: 99%

Insights into Planet Formation from Debris Disks

Wyatt

Jackson

2016

Space Sci Rev

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Giant impacts refer to collisions between two objects each of which is massive enough to be considered at least a planetary embryo. The putative collision suffered by the proto-Earth that created the Moon is a prime example, though most Solar System bodies bear signatures of such collisions. Current planet formation models predict that an epoch of giant impacts may be inevitable, and observations of debris around other stars are providing mounting evidence that giant impacts feature in the evolution of many planetary systems. This chapter reviews giant impacts, focussing on what we can learn about planet formation by studying debris around other stars. Giant impact debris evolves through mutual collisions and dynamical interactions with planets. General aspects of this evolution are outlined, noting the importance of the collision-point geometry. The detectability of the debris is discussed using the example of the Moon-forming impact. Such debris could be detectable around another star up to 10 Myr post-impact, but model uncertainties could reduce detectability to a few 100 yr window. Nevertheless the 3 % of young stars with debris at levels expected during terrestrial planet formation provide valuable constraints on formation models; implications for super-Earth formation are also discussed. Variability recently observed in some bright disks promises to illuminate the evolution during the earliest phases when vapour condensates may be optically thick and acutely affected by the collision-point geometry. The outer reaches of planetary systems may also exhibit signatures of giant impacts, such as the clumpy debris structures seen around some stars.

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“…We defined the production rate of first-generation Veritas particles as P (D,t), where D is diameter and t is the elapsed time since the family formed. Motivated by results from main belt collisional evolution models 9 , we assumed P(D,t) has a segmented cumulative power-law size frequency distribution with index α 1 in the interval (Dmin,Dbreak) and α 2 in the interval (Dbreak,Dmax). We assumed that collisional and dynamical evolution causes P(D,t) to vary such that Dbreak, the diameter at which the power-law slope changes, increases with time according to: The particles were started at heliocentric distance 3.17 AU.…”

Section: Monte Carlo Dust Evolution Modelmentioning

confidence: 99%

“…The former values are shallower than the canonical value of -2.5 (ref 13) because P-R drag quickly removes small particles from the main belt, while the latter values are steeper because we need to link our size distribution to the observed members of the Veritas family while also conserving mass. We also tested values of τ decay = 0.5, 0.75, and 1 Myr, where the timescales were drawn from collision code experiments 9 .…”

Section: Monte Carlo Dust Evolution Modelmentioning

confidence: 99%

A late Miocene dust shower from the break-up of an asteroid in the main belt

Farley

Vokrouhlický

Bottke

et al. 2006

Nature

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A Late Miocene dust shower from the break-up of an asteroid in the main belt SamplesCarbonate sediments were studied from two deep sea cores. A suite of samples spanning from the middle Eocene to ~3 Ma was obtained from Hole 757B in the central Indian Ocean, 17°01.458'S, 88°10.899'E, on the Ninety East Ridge. This hole was cored on Leg 121 of the Ocean Drilling Program and has been described in detail 1 . Over the studied time interval this site is thought to have subsided from a Middle Eocene depth of ~1500 m to its present depth of 1650 m. Sediments from this site are extremely pure carbonate oozes (usually >95% CaCO 3 ) that have accumulated at a fairly slow average rate of 0.35 cm/kyr. The purpose of this suite was to identify any intervals worthy of more detailed study at sites with faster accumulation rates and hence higher temporal resolution. ~140 samples were analyzed at about 1 meter intervals from ~18 to ~ 135 mbsf, except in two areas of interest, in the Late Eocene and the Late Miocene, where sampling density was higher.Based on elevated extraterrestrial 3 He concentrations in the Late Miocene an additional suite of samples was obtained from amongst the best studied cores spanning this interval, from Hole 926B. This hole was drilled on the Ceara Rise, western equatorial Atlantic (3 o 43.148'N, 42 o 54.507'W, 3600 m water depth) on Leg 154 of the Ocean Drilling Program 2 . The Late Miocene interval is a clayey carbonate ooze (~65% CaCO 3 ) with a mean accumulation rate of ~1.7 cm/kyr. 73 samples were analyzed in the interval between 159 and 224 mbsf. The spacing of these samples is ~ 1.5 meters away from the 3 He peak to as close as a few cm at the peak. MethodsSamples were analyzed for helium isotopes following removal of CaCO 3 using standard procedures at Caltech 3 . In all cases 3 He and 4 He blank levels were sufficiently low compared to sample signals that blank corrections were not required. Many samples were analyzed in duplicate to detect and eliminate anomalously high 3 He values arising from occasional over-sampling of large IDP grains 4 . When preparing the final 3 He and 3 He/ 4 He data set the following procedure was adopted for incorporating replicated analyses. If the duplicates agreed to within a factor of three, the average was used. If the difference exceeded a factor of three, the higher value was excluded. This led to exclusion of about 6% of the 3 He measurements. For 4 He and non-carbonate fraction data the replicates were simply averaged. Age Models Site 757The age model for site 757 comes primarily from shipboard biostratigraphy. Event locations are from the shipboard report 1 with updated datum ages from Backman and Raffi 5 . To facilitate comparison with previous wok at the Massignano GSSP,

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The fossilized size distribution of the main asteroid belt

Cited by 535 publications

References 124 publications

Formation of brown dwarfs and planets

Formation of brown dwarfs and planets

Insights into Planet Formation from Debris Disks

A late Miocene dust shower from the break-up of an asteroid in the main belt

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