Parent bodies of the meteorites and the origin of chondrules

Urey, Harold C.

doi:10.1016/0019-1035(67)90079-6

Cited by 53 publications

(19 citation statements)

References 32 publications

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“…Alternatively, crystalline silicates can be formed in situ in the outer disk by shock waves (Harker & Desch 2002;Desch et al 2005), lightning (e.g. Pilipp et al 1998), parent-body collisions (Urey 1967;Huss et al 2001;Morlok et al 2010), and stellar outbursts (Juhász et al 2012). To understand the significance of these scenarios, it is important to characterise the location, composition, and sizes of forsterite grains in protoplanetary disks.…”

Section: Discussionmentioning

confidence: 99%

“…This may reflect the lack of large-scale mixing (Shu et al 1994;Bockelée-Morvan et al 2002;Gail 2004;Jacquet 2014) and indicates the importance of crystal formation (i.e. local heating events) associated with the inner and outer disk region (Urey 1967;Huss et al 2001;Harker & Desch 2002;Desch et al 2005;Ábrahám et al 2009;Morlok et al 2010;Tanaka et al 2010).…”

Section: Introductionmentioning

confidence: 99%

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Location and sizes of forsterite grains in protoplanetary disks

Maaskant

Vries

Min

et al. 2015

A&A

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Context. The spectra of protoplanetary disks contain mid-and far-infrared emission features produced by forsterite dust grains. The spectral features contain information about the forsterite temperature, chemical composition and grain size. Aims. We aim to characterize how the 23 and 69 µm features can be used to constrain the physical locations of forsterite in disks. We check for consistency between two independent forsterite temperature measurements: the I 23 /I 69 feature strength ratio and the shape of the 69 µm band. Methods. We performed radiative transfer modeling to study the effect of disk properties to the forsterite spectral features. Temperature-dependent forsterite opacities were considered in self-consistent models to compute forsterite emission from protoplanetary disks. Results. Modelling grids are presented to study the effects of grain size, disk gaps, radial mixing and optical depth to the forsterite features. Independent temperature estimates derived from the I 23 /I 69 feature strength ratio and the 69 µm band shape are most inconsistent for HD 141569 and Oph IRS 48. A case study of the disk of HD 141569 shows two solutions to fit the forsterite spectrum. A model with T ∼ 40 K, iron-rich (∼0−1% Fe) and 1 µm forsterite grains, and a model with warmer (T ∼ 100 K), iron-free, and larger (10 µm) grains. Conclusions. We find that for disks with low upper limits of the 69 µm feature (most notably in flat, self-shadowed disks), the forsterite must be hot, and thus close to the star. We find no correlation between disk gaps and the presence or absence of forsterite features. We argue that the 69 µm feature of the evolved transitional disks HD 141569 and Oph IRS 48 is most likely a tracer of larger (i.e. 10 µm) forsterite grains.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Location and sizes of forsterite grains in protoplanetary disks

Maaskant

Vries

Min

et al. 2015

A&A

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“…Production of chondrules as melt droplets produced during collisions of asteroids has long been suggested (Urey and Craig 1953; Urey 1967; Sanders 1996; Sanders and Taylor 2005; Asphaug et al. 2011).…”

Section: Chondrule Formation Modelsmentioning

confidence: 99%

“…1996, 1997, 2001) or by ablation in the bipolar outflow that accompanies the proto‐Sun (Skinner 1990; Liffman and Brown 1996; Liffman 2009). Some models identify chondrules as melt droplets produced during collisions between planetary bodies (Urey and Craig 1953; Urey 1967; Sanders 1996; Sanders and Taylor 2005; Asphaug et al. 2011).…”

Section: Introductionmentioning

confidence: 99%

The importance of experiments: Constraints on chondrule formation models

Desch

Morris

Connolly

et al. 2012

Meteorit & Planetary Scien

135

134

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Abstract-We review a number of constraints that have been placed on the formation of chondrules and show how these can be used to test chondrule formation models. Four models in particular are examined: the ''X-wind'' model (sudden exposure to sunlight <0.1 AU from the proto-Sun, with subsequent launching in a magnetocentrifugal outflow); solar nebula lightning; nebular shocks driven by eccentric planetesimals; and nebular shocks driven by diskwide gravitational instabilities. We show that constraints on the thermal histories of chondrules during their melting and crystallization are the most powerful constraints and provide the least ambiguous tests of the chondrule formation models. Such constraints strongly favor melting of chondrules in nebular shocks. Shocks driven by gravitational instabilities are somewhat favored over planetesimal bow shocks.

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“…Urey has argued that there are several observed facts in some meteorites that require the presence of a gravitational field such as would be found near or on the surface of the moon, or in general an object considerably larger than a 200-km radius asteroid. (For recent discussions, see Urey [1965Urey [ , 1966Urey [ , 1967 and Urey and Marti [1968].) Is it possible that A12• was produced in situ in the feldspar grains by high-energy proton irradiation of the surface of a planet?…”

Section: Hydrocarbons C•it• Was Always Monitored During Analyses Anmentioning

confidence: 99%

Aluminum 26-magnesium 26 dating of feldspar in meteorites

Clarke¹,

Laeter²,

Schwarcz³

et al. 1970

J. Geophys. Res.

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A search for ‘fossil’ Mg26 from the decay of 0.72 m.y. Al26 in an aluminum‐rich (plagioclase feldspar) phase of several stone meteorites has been carried out. An electron impact ion source in a tandem mass spectrometer was used for a series of measurements of the relative abundances of table magnesium isotopes in meteoritic and terrestrial feldspar, as well as in unseparated (‘common’) magnesium from meteorites, from meteoritic chondrules, and from laboratory reagents. Relative to terrestrial magnesium, the meteorites Bruderheim and Khor Temiki show a definite Mg26 excess (4–6‰). Haraiya and Mocs also show this effect although the experimental evidence is not nearly as secure as in the first two examples; Moore County is a borderline case. Magnesium contents of the separated feldspar phases were measured by isotope dilution, allowing a calculation of Mg26 (radiogenic), relative to Si = 106 atoms for the meteorites. The following conclusions can be made: (1) the feldspar of some meteorites cooled to below the temperature of appreciable Mg diffusion (∼650°C) within a time spread of about 3 m.y.; (2) only a short time (≤5 m.y.) could have elapsed between the end of Al26 production and formation of the feldspar phase in some meteorites; (3) the process that produced Al26 early in the history of the solar system (most probably solar proton irradiation of surrounding material) was of short duration (<5 m.y.); (4) if the levels of Al26 deduced from measurements of excess Mg26 were present at the time of formation of objects a few tens of km in radius, sufficient energy would have been produced by radioactive decay of Al26 to heat the centers of these objects to near their melting points.

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Parent bodies of the meteorites and the origin of chondrules

Cited by 53 publications

References 32 publications

Location and sizes of forsterite grains in protoplanetary disks

Location and sizes of forsterite grains in protoplanetary disks

The importance of experiments: Constraints on chondrule formation models

Aluminum 26-magnesium 26 dating of feldspar in meteorites

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