Do comets have chondrules and CAIs? Evidence from the Leonid meteors

Swindle, T. D.; Campins, H.

doi:10.1111/j.1945-5100.2004.tb00069.x

Cited by 11 publications

(8 citation statements)

References 46 publications

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“…Fig. 5a), on the other hand, might well be explained in terms of cluster aggregated meteoroids (Murray et al 2000; Swindle & Campins 2004). Those light curves showing flares are presumably telling us something about the thermal fragmentation and/or crumbling of the larger fundamental grains.…”

Section: Discussionmentioning

confidence: 93%

The classification of meteor light curves: an application of hat theory

Beech¹

2007

Monthly Notices of the Royal Astronomical Society

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A three‐component, geometrical classification scheme for meteor light curves is developed and presented. A fundamental distinction between convex and non‐convex light‐curve profiles is first made, and then the individual light curves are quantified according to the relative trail‐length location of the point of maximum brightness, and the area under the light curve in the normalized magnitude versus time diagram. It is argued that the proposed scheme, while geometrical in nature, does have contact with the theoretical models of meteoroid ablation in the sense that the most extreme profiles or bounding light curves (called ‘hats’ for convenience) correspond to very specific modes of material mass loss.

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Section: Discussionmentioning

confidence: 93%

The classification of meteor light curves: an application of hat theory

Beech¹

2007

Monthly Notices of the Royal Astronomical Society

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“…The recent preliminary detection of hydrous silicates in comet Temple 1 by the Deep Impact mission (unpublished press release), however, indicates that some FgMMs and even CI chondrites may have a cometary origin (Gounelle et al 2004(Gounelle et al , 2006Lodders and Osborne 1999;McSween and Weissman 1989). The occurrence of chondrules and refractory inclusions within cometary materials has also been postulated to explain rare dense compact particles observed within cometary meteor streams (Swindle and Campins 2004) and is not precluded by models of the transport of these objects in the early solar system such as the X-wind model (Shu et al 2001). The presence of chondrule or CAI fragments in MMs, therefore, is not conclusive evidence of an asteroidal origin.…”

Section: Discussionmentioning

confidence: 99%

The classification of micrometeorites

Genge

Engrand

Gounelle

et al. 2008

Meteorit & Planetary Scien

223

373

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Abstract-Due to their small size, the mineralogical and chemical properties of micrometeorites (MMs) are not representative of their parent bodies on the centimeter to meter scales that are used to define parent body groups through the petrological study of meteorites. Identifying which groups of MM are derived from the same type of parent body is problematic and requires particles to be rigorously grouped on the basis of mineralogical, textural, and chemical properties that reflect the fundamental genetic differences between meteorite parent bodies, albeit with minimal bias towards preconceived genetic models. Specifically, the interpretation of MMs requires a rigorous and meaningful classification scheme. At present the classification of MMs is, however, at best ambiguous. A unified petrological-chemical classification scheme is proposed in the current study and is based on observations of several thousand MMs collected from Antarctic ice.

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“…The size was of the order of 1 mm. Swindle & Campins (2004) speculated whether this is an evidence for presence of chondrules in cometary matter but considered it unlikely. Rather, this can be regarded as a piece of evidence for the opinion expressed by various authors (see e.g.…”

Section: Cometary Meteoroidsmentioning

confidence: 99%

Physical and chemical properties of meteoroids as deduced from observations

Borovička

2005

Proc. IAU

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A review of the current knowledge of physical properties and chemical composition of meteoroids entering the Earth's atmosphere is presented. Meteoroid penetration ability, ablation coefficients, beginning heights, light curves, fragmentation, and spectra are considered. The inferred bulk densities, mechanical strengths, rotation, and atomic elemental abundances are discussed. Cometary meteoroids are effectively grain aggregates with low bulk density (100-1000 kg m −3), high porosity and low cohesivity. A volatile matrix holding the grains together may be present. Presence of large amounts of organic material is not firmly established. Small chunks (∼1 mm) of denser material are sometimes contained in cometary meteoroids. Chemically, cometary grains are similar to CI chondrites but there is a hint of enhancement of Na, Si, and Mg and depletion of Fe, Cr, and Mg. Larger chemical diversity is observed among small meteoroids on cometary orbits not belonging to meteoroid streams. The relatively frequent Na-free meteoroids are probably fragments of cometary irradiation crust. Asteroidal meteoroids exhibit much lower mechanical strengths than stony meteorites, clearly due to the presence of large scale cracks. Iron meteoroids dominate among asteroidal meteoroids smaller than 1 cm.

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Do comets have chondrules and CAIs? Evidence from the Leonid meteors

Cited by 11 publications

References 46 publications

The classification of meteor light curves: an application of hat theory

The classification of meteor light curves: an application of hat theory

The classification of micrometeorites

Physical and chemical properties of meteoroids as deduced from observations

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