Post-Impact Thermal Evolution of Porous Planetesimals. Davison, T. M., Ciesla, F. J., & Collins, G. S. Geochimica et Cosmochimica Acta, 95:252–269, 2012. ![Post-Impact Thermal Evolution of Porous Planetesimals [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex Impacts between planetesimals have largely been ruled out as a heat source in the early Solar System, by calculations that show them to be an inefficient heat source and unlikely to cause global heating. However, the long-term, localized thermal effects of impacts on planetesimals have never been fully quantified. Here, we simulate a range of impact scenarios between planetesimals to determine the post-impact thermal histories of the parent bodies, and hence the importance of impact heating in the thermal evolution of planetesimals. We find on a local scale that heating material to petrologic type 6 is achievable for a range of impact velocities and initial porosities, and impact melting is possible in porous material at a velocity of > 4 km/s. Burial of heated impactor material beneath the impact crater is common, insulating that material and allowing the parent body to retain the heat for extended periods (∼ millions of years). Cooling rates at 773 K are typically 1 - 1000 K/Ma, matching a wide range of measurements of metallographic cooling rates from chondritic materials. While the heating presented here is localized to the impact site, multiple impacts over the lifetime of a parent body are likely to have occurred. Moreover, as most meteorite samples are on the centimeter to meter scale, the localized effects of impact heating cannot be ignored.
@article{davison_post-impact_2012,
title = {Post-{Impact} {Thermal} {Evolution} of {Porous} {Planetesimals}},
volume = {95},
issn = {0016-7037},
url = {http://www.sciencedirect.com/science/article/pii/S0016703712004486?v=s5},
doi = {10.1016/j.gca.2012.08.001},
abstract = {Impacts between planetesimals have largely been ruled out as a heat source in the early Solar System, by calculations that show them to be an inefficient heat source and unlikely to cause global heating. However, the long-term, localized thermal effects of impacts on planetesimals have never been fully quantified. Here, we simulate a range of impact scenarios between planetesimals to determine the post-impact thermal histories of the parent bodies, and hence the importance of impact heating in the thermal evolution of planetesimals. We find on a local scale that heating material to petrologic type 6 is achievable for a range of impact velocities and initial porosities, and impact melting is possible in porous material at a velocity of \> 4 km/s. Burial of heated impactor material beneath the impact crater is common, insulating that material and allowing the parent body to retain the heat for extended periods (∼ millions of years). Cooling rates at 773 K are typically 1 - 1000 K/Ma, matching a wide range of measurements of metallographic cooling rates from chondritic materials. While the heating presented here is localized to the impact site, multiple impacts over the lifetime of a parent body are likely to have occurred. Moreover, as most meteorite samples are on the centimeter to meter scale, the localized effects of impact heating cannot be ignored.},
urldate = {2012-08-17},
journal = {Geochimica et Cosmochimica Acta},
author = {Davison, Thomas M. and Ciesla, Fred J. and Collins, Gareth S.},
year = {2012},
pages = {252--269},
}
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