The impact origin of Eunomia and Themis families

Leliwa-Kopystyński, J.; Burcheli, M. J.; Włdarczyk, I.

doi:10.1111/j.1945-5100.2009.tb02002.x

Cited by 10 publications

(4 citation statements)

References 27 publications

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Section: Eunomia Familymentioning

confidence: 99%

“…The Eunomia family is the largest family in the intermediate part of the main belt, with an estimated >4,500 members (Leliwa-Kopystński et al 2009). Unlike the Eos parent asteroid, the inferred ∼300-km-diameter Eunomia family parent asteroid is thought to have remained mostly intact as the present-day 264-km-diameter S-type asteroid 15 Eunomia (Leliwa-Kopystński et al 2009). 15 Eunomia appears to have a compositionally variegated surface, with one face resembling stony-iron meteorites (olivine-and possibly also metal-rich) and the opposite face more basaltic (pyroxene-rich) (Nathues 2010).…”

Section: Eunomia Familymentioning

confidence: 99%

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Differentiated Planetesimals and the Parent Bodies of Chondrites

Weiss

Elkins-Tanton

2013

Annu. Rev. Earth Planet. Sci.

136

105

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Meteorites are samples of dozens of small planetary bodies that formed in the early Solar System. They exhibit great petrologic diversity, ranging from primordial accretional aggregates (chondrites), to partially melted residues (primitive achondrites), to once fully molten magmas (achondrites). It has long been thought that no single parent body could be the source of more than one of these three meteorite lithologies. This view is now being challenged by a variety of new measurements and theoretical models, including the discovery of primitive achondrites, paleomagnetic analyses of chondrites, thermal modeling of planetesimals, the discoveries of new metamorphosed chondrites and achondrites with affinities to some chondrite groups, and the possible identification of extant partially differentiated asteroids. These developments collectively suggest that some chondrites could in fact be samples of the outer, unmelted crusts of otherwise differentiated planetesimals with silicate mantles and metallic cores. This may have major implications for the origin of meteorite groups, the meaning of meteorite paleomagnetism, the rates and onset times of accretion, and the interior structures and histories of asteroids.

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Section: Eunomia Familymentioning

confidence: 99%

Section: Eunomia Familymentioning

confidence: 99%

Differentiated Planetesimals and the Parent Bodies of Chondrites

Weiss

Elkins-Tanton

2013

Annu. Rev. Earth Planet. Sci.

136

105

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“…Statistically speaking, smaller asteroids tend to be younger than larger asteroids within the same family. For example, the Themis family is an old family (∼2.5 Gyr) that has likely experienced multiple disruption events (Nesvornỳ et al 2003;Leliwa-Kopystyński et al 2009). Smaller objects resulting from later disruption events would have younger surfaces than older, larger objects in the sense that they have experienced less space weathering and thermal fatigue, both of which are processes that would cause the breakdown of surface particles into finer grains.…”

Section: Discussionmentioning

confidence: 99%

3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry

Varakian,

Chanover,

Masiero

et al. 2024

Planet. Sci. J.

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The shapes of asteroid phase curves are influenced by the physical properties of asteroid surfaces. The variation of an asteroid’s brightness as a function of the solar phase angle can tell us about surface properties such as grain size distribution, roughness, porosity, and composition. Phase curves are traditionally derived from photometric observations at visible wavelengths, but phase curves using infrared data can also provide useful information about an asteroid surface. Using photometric observations centered near ∼3.4 μm from the W1 band of the Near-Earth Object Wide-field Infrared Survey Explorer mission, we construct thermally and rotationally corrected infrared phase curves for a sample of main-belt asteroids, which includes asteroids observed by the AKARI satellite, as well as subsets of the Themis and Flora dynamical families. We calculate the linear slope of the phase curves as a measure of their shape and compare W1 phase slopes to band depths of absorption features associated with hydrated materials, spectral slopes, visible albedos, W1 albedos, and diameters. We observe a steepening of the W1 phase slope of C-type asteroids with increasing 2.7 μm band depth but little correlation between the phase slope and 3 μm band depth or 3 μm spectral slope. The C-types in our sample exhibit steeper average W1 phase slopes than M- or S-types, similar to visible-light phase slopes. We also observe steeper W1 phase slopes for smaller-diameter objects within the Themis family and explore comparisons to Jupiter-family comets in phase slope versus albedo space.

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“…(Compare table of Leliwa‐Kopystynski et al. , based on a data set containing only 205,770 asteroids. However, in that table, the populations of families were erroneously displaced: it should be 9000 for Eunomia and 4500 for Themis.…”

Section: Application Of Hcm For Five Selected Familiesmentioning

confidence: 99%

Volume and mass distribution in selected asteroid families

Wlodarczyk¹,

Leliwa-Kopystyński

2014

Meteorit & Planetary Scien

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The main focus of this paper is calculation of the diameters of asteroids belonging to five families (Vesta, Eos, Eunomia, Koronis, and Themis). To do that, we used the HCM algorithm applied for a data set containing 292,003 numbered asteroids, and a numerical procedure for choosing the crucial parameter of the HCM, called "the cutting velocity" v cut . It was established with a precision as high as 1 m s À1 . Thereafter, we used the WISE (Widefield Infrared Survey Explorer) catalog to set a range of albedo for the largest members of each family considered. The albedo data were supported by the data concerning color classification (SDSS MOC4). The asteroids with albedo out of this range were classified as interlopers and were therefore disqualified as family members. Sizes were calculated for the asteroids with albedo within the acceptable range. For the other asteroids (those chosen by means of the HCM, but with albedo not listed in the WISE), the value of albedo of the largest member of the family was adopted. Results are given in a set of figures showing the families on the planes (a, e), (a, i), (e, i). Diameters and volumes of the asteroids that are the individual members of a family were calculated on the basis of their known or assumed albedo and on their absolute magnitude. Volumes of the parent bodies of the families were found on the basis of the cumulative volume distribution of these families. We also studied the secular resonances of the family members. We have shown that the locations of members of the considered asteroid families are related to the lines of secular resonances z 1 , z 2 , and z 3 with Saturn.

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The impact origin of Eunomia and Themis families

Cited by 10 publications

References 27 publications

Differentiated Planetesimals and the Parent Bodies of Chondrites

Differentiated Planetesimals and the Parent Bodies of Chondrites

3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry

Volume and mass distribution in selected asteroid families

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