The common origin of family and non-family asteroids

Dermott, S. F.; Christou, Apostolos; Li, Dan; Kehoe, T. J. J.; Robinson, J. Malcolm

doi:10.1038/s41550-018-0482-4

Cited by 40 publications

(35 citation statements)

References 22 publications

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“…However, consistent with various previous studies Deienno et al 2016;Clement et al 2018;Deienno et al 2018), our simulations often fail to replicate the AB's population about the ν 6 secular resonance. However, the MB size distribution has evolved significantly since the epoch of terrestrial planet formation (Bottke et al 2005a), and its orbital distribution has likely been altered via the formation of collisional families (Dermott et al 2018). Since the MB's mass profile is dominated by just a few asteroids, one of which (Pallas) is on a highly inclined orbit above the ν 6 resonance, our systems still broadly replicate the distribution of the most massive asteroids.…”

Section: The Formation Of Veneneiamentioning

confidence: 81%

“…However, the MB's radial mass distribution profile is far from uniform because half of its mass is concentrated in just 4 asteroids. From the standpoint of mass distribution, the MB's structure seems to be better characterized by just a handful of massive bodies embedded in a sea of objects several orders of magnitude smaller (many of which are likely the products of collisional grinding; Bottke et al (2005aBottke et al ( , 2015; Dermott et al (2018)). Indeed, the ν 6 ratio calculated for all known asteroids with a<2.8 au with respect to number of asteroids (0.04), is a significantly smaller than when it is calculated with respect to mass (0.14).…”

Section: Orbital Structurementioning

confidence: 99%

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Excitation and Depletion of the Asteroid Belt in the Early Instability Scenario

Clement

Raymond

Kaib

2019

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Containing only a few percent the mass of the moon, the current asteroid belt is around three to four orders of magnitude smaller that its primordial mass inferred from disk models. Yet dynamical studies have shown that the asteroid belt could not have been depleted by more than about an order of magnitude over the past ∼4 Gyr. The remainder of the mass loss must have taken place during an earlier phase of the solar system's evolution. An orbital instability in the outer solar system occurring during the process of terrestrial planet formation can reproduce the broad characteristics of the inner solar system. Here, we test the viability of this model within the constraints of the main belt's low present-day mass and orbital structure. While previous studies modeled asteroids as massless test particles because of limited computing power, our work uses GPU (Graphics Processing Unit) acceleration to model a fully self-gravitating asteroid belt. We find that depletion in the main belt is related to the giant planets' exact evolution within the orbital instability. Simulations that produce the closest matches to the giant planets' current orbits deplete the main belt by two to three orders of magnitude. These simulated asteroid belts are also good matches to the actual asteroid belt in terms of their radial mixing and broad orbital structure.

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Section: The Formation Of Veneneiamentioning

confidence: 81%

Section: Orbital Structurementioning

confidence: 99%

Excitation and Depletion of the Asteroid Belt in the Early Instability Scenario

Clement

Raymond

Kaib

2019

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“…They will also mostly still have an inclination close to that of the source asteroid. Asteroid families, as well as large asteroids, have the most surface area for collisions, more so than the background asteroids (Dermott et al 2018). That identifies a discrete number of potential source regions for the individual CRE peaks in Fig.…”

Section: Methodsmentioning

confidence: 88%

Review of asteroid-family and meteorite-type links

Jenniskens

2018

Proc. IAU

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The materials of large asteroids and asteroid families are sampled by meteorites that fall to Earth. The cosmic ray exposure age of the meteorite identifies the collision event from which that meteorite originated. The inclination of the orbit on which the meteoroid impacted Earth measures the inclination of the source region, while the semi-major axis of the orbit points to the delivery resonance, but only in a statistical sense. To isolate the sources of our meteorites requires multiple documented falls for each cosmic ray exposure peak. So far, only 36 meteorites have been recovered from observed falls. Despite these low numbers, some patterns are emerging that suggest CM chondrites originated from near the 3:1 resonance from a low-inclined source (perhaps the Sulamitis family), LL chondrites came to us from the ν6 resonance (perhaps the Flora family), there is an H chondrite source at high inclination (Phocaea?), and one group of low shock-stage L chondrites originates from the inner main belt. Other possible links are discussed.

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“…Summarizing, in the real world the family search is done in parts of the asteroid belt that may contain both family members and background population. The asteroid belt itself could be entirely composed of members of unidentified families (Dermott et al, 2018). These aspects of the real asteroid belt, along with the possibility of misleading signals due to edge effects, precisely reflect why we need to understand and characterize the searching tools.…”

Section: Need For Calibrationmentioning

confidence: 99%

“…We need to integrate a larger population of asteroids under the influence of the planets in order to capture the complex dynamics of the main belt to be sure not to overestimate the behavior of the algorithms by under-estimating the orbital complexity of the asteroid belt. Note that one possible scenario for the actual main belt is that the background is composed entirely of old families (Dermott et al, 2018); precisely why we are building the synthetic background via direct integration.…”

Section: Synthetic Backgroundmentioning

confidence: 99%

Efficiency characterization of the V-shape asteroid family detection method

Deienno

Walsh

Delbò

2021

Icarus

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Following the break up of a parent body, the Yarkovsky effect causes asteroid family members to spread in orbital semimajor axis with a rate often inversely proportional to their diameter. This size dependent semimajor axis drift causes family members to form structures in the semimajor axis vs inverse diameter plane that have the shape of the letter V. The V-shape method consists in finding the borders of such V-shapes of unknown center and opening. Although successfully employed to find some very old families in the inner main asteroid belt, the V-shape searching method is very sensitive to many parameters. In this work, we first created and evolved a synthetic asteroid family over billions of years. Then, by adding uncertainties to semimajor axis and diameter of the evolved synthetic family components, we randomly generated additional 99 similar, but not perfectly V-shaped, family clones. We chose a fairly low initial velocity dispersion of 20 m/s for our family. Thus, we can more easily relate the spreading in semimajor axis with the family's age (slope of the evolving V). A synthetic background with an initially randomly distributed components was also created and evolved for 100 Myr. Thus, by setting different levels of ratio of the synthetic family and background asteroids, we derived a detection efficiency map for the V-shape method and determined how sensitive the results can be based on signal-to-noise levels. We also determined optimal parameter values for the method's efficiency. We found that, families older than ≈3 Gyr are likely undetectable, with a method efficiency of 50% or less, whereas younger families (0.5-2.5 Gyr) are more easily detected by the method, with an efficiency of ≳80%.

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The common origin of family and non-family asteroids

Cited by 40 publications

References 22 publications

Excitation and Depletion of the Asteroid Belt in the Early Instability Scenario

Excitation and Depletion of the Asteroid Belt in the Early Instability Scenario

Review of asteroid-family and meteorite-type links

Efficiency characterization of the V-shape asteroid family detection method

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