Thermal evolution and sintering of chondritic planetesimals

Gail, H. P.; Henke, Stephan; Trieloff, M.

doi:10.1051/0004-6361/201424278

Cited by 28 publications

(43 citation statements)

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“…This research has made use of NASA's Astrophysics Data System. The matrix re-crystallizes and sinters already at lower pressures and temperatures by surface diffusion (Gail et al 2015). According to our sinter model the initially fine grained matrix starts to coarsen and sinter at temperatures between 520 and 550 K, see Fig.…”

mentioning

confidence: 67%

“…Here we apply the sinter model of Helle et al (1985). The application of this model to parent bodies of ordinary chondrites is discussed in Gail et al (2015); it requires to solve a differential equation for Φ simultaneously with the heat conduction equation. The pressure p required for calculating the sintering process is determined by the hydrostatic equilibrium equation…”

Section: Equationsmentioning

confidence: 99%

“…At the same time its mineral composition is equilibrated. We include the process of compaction in our thermal evolution model of the L chondrite parent body in the same way as described in Gail et al (2015) for the case of the evolution of the H chondrite parent body. The calculation is based on a theory of isostatic hot pressing used for the modelling of sintering in technical processes.…”

Section: Appendix A5: Sinteringmentioning

confidence: 99%

“…The calculation is based on a theory of isostatic hot pressing used for the modelling of sintering in technical processes. All necessary equations and input data are described in Gail et al (2015). We have only to observe that the average chondrule diameter in L chondrites is with 0.5 mm bigger than the average diameter of 0.3 mm for chondrules in H chondrites.…”

Section: Appendix A5: Sinteringmentioning

confidence: 99%

“…This saves much computing time. The prescription is guided by experience with complete numerical simulations of the sintering process (Gail et al 2015) that in models for chondrite parent bodies the loss of porosity by sintering occurs over a rather narrow temperature interval. The prescription mimics this by switching in a continuous fashion between the limit cases of low-conductivity for porous material and high-conductivity for compacted material within the temperature interval from T sl to T sh .…”

Section: Appendix A5: Sinteringmentioning

confidence: 99%

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Thermal history modelling of the L chondrite parent body

Gail

Trieloff

2019

A&A

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Context. The cooling history of individual meteorites can be reconstructed if closure temperatures and closure ages of different radioisotopic chronometers are available for a couple of meteorites. If a high similarity of chemical and isotopic composition suggests a common origin from the same parent body, some basic properties of this body can be derived. Aims. The radius of the L chondrite parent body, its formation time, and its evolution history are determined by fitting theoretical models to empirical data of radioisotopic chronometers for L chondrites. Methods. A simplified evolution model for the L chondrite parent body is constructed considering sintering of the initially porous material, temperature dependent heat conductivity, and an insulating regolith layer. Such models are fitted to thermochronological data of five meteorites for which precise data for the Hf-W and U-Pb-Pb thermochronometers have been published. Results. A set of parameters for the L chondrite parent body is found that yields excellent agreement (within error bounds) between a thermal evolution model and thermochonological data of five examined L chondrites. Empirical cooling rate data also agree with the model results within error bounds such that there is no conflict between cooling rate data and the onion-shell model. Two models are found to be compatible with the presently available empirical data: One model with a radius of 115 km and a formation time of 1.89 Ma after CAI formation, another model with 160 km radius and formation time of 1.835 Ma. The central temperature of the smaller body remains well below the Ni,Fe-FeS eutectic melting temperature and is consistent with the apparent non-existence of primitive achondrites related to the L chondrites. For the bigger model incipient melting in the central core region is predicted which opens the possibility that primitive achondrites related to L chondrites could be found.

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confidence: 67%

Section: Equationsmentioning

confidence: 99%

Section: Appendix A5: Sinteringmentioning

confidence: 99%

Section: Appendix A5: Sinteringmentioning

confidence: 99%

Section: Appendix A5: Sinteringmentioning

confidence: 99%

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Thermal history modelling of the L chondrite parent body

Gail

Trieloff

2019

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Possible thermal evolutionary pathways of irregular shaped small asteroids and planetesimals

Sahijpal

2022

J Earth Syst Sci

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Late metal–silicate separation on the IAB parent asteroid: Constraints from combined W and Pt isotopes and thermal modelling

Hunt

Cook

Lichtenberg

et al. 2018

Earth and Planetary Science Letters

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The short-lived 182 Hf-182 W decay system is a powerful chronometer for constraining the timing of metal-silicate separation and core formation in planetesimals and planets. Neutron capture effects on W isotopes, however, significantly hamper the application of this tool. In order to correct for neutron capture effects, Pt isotopes have emerged as a reliable in-situ neutron dosimeter. This study applies this method to IAB iron meteorites, in order to constrain the timing of metal segregation on the IAB parent body.The ε 182 W values obtained for the IAB iron meteorites range from −3.61 ± 0.10 to −2.73 ± 0.09. Correlating ε i Pt with ε 182 W data yields a pre-neutron capture ε 182 W of −2.90 ± 0.06. This corresponds to a metal-silicate separation age of 6.0 ± 0.8 Ma after CAI for the IAB parent body, and is interpreted to represent a body-wide melting event. Later, between 10 and 14 Ma after CAI, an impact led to a catastrophic break-up and subsequent reassembly of the parent body. Thermal models of the interior evolution that are consistent with these estimates suggest that the IAB parent body underwent metalsilicate separation as a result of internal heating by short-lived radionuclides and accreted at around 1.4 ± 0.1 Ma after CAIs with a radius of greater than 60 km.

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Thermal evolution and sintering of chondritic planetesimals

Cited by 28 publications

References 50 publications

Thermal history modelling of the L chondrite parent body

Thermal history modelling of the L chondrite parent body

Possible thermal evolutionary pathways of irregular shaped small asteroids and planetesimals

Late metal–silicate separation on the IAB parent asteroid: Constraints from combined W and Pt isotopes and thermal modelling

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