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    The formation of the Baptistina family by catastrophic disruption: Porous versus non-porous parent body

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    Author
    Jutzi, M.
    Michel, P.
    Benz, W.
    Richardson, D. C.
    Issue Date
    2009-01-01
    Keywords
    asteroid disruption
    asteroid families
    asteroid meteorite links
    porosity
    
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    Citation
    Jutzi, M., Michel, P., Benz, W., & Richardson, D. C. (2009). The formation of the Baptistina family by catastrophic disruption: Porous versus non‐porous parent body. Meteoritics & Planetary Science, 44(12), 1877-1887.
    Publisher
    The Meteoritical Society
    Journal
    Meteoritics & Planetary Science
    URI
    http://hdl.handle.net/10150/656651
    DOI
    10.1111/j.1945-5100.2009.tb01997.x
    Additional Links
    https://meteoritical.org/
    Abstract
    In this paper, we present numerical simulations aimed at reproducing the Baptistina family based on its properties estimated by observations. A previous study by Bottke et al. (2007) indicated that this family is probably at the origin of the K/T impactor, is linked to the CM meteorites and was produced by the disruption of a parent body 170 km in size due to the head-on impact of a projectile 60 km in size at 3 km s^(-1). This estimate was based on simulations of fragmentation of non-porous materials, while the family was assumed to be of degrees C taxonomic type, which is generally interpreted as being formed from a porous body. Using both a model of fragmentation of non-porous materials, and a model that we developed recently for porous ones, we performed numerical simulations of disruptions aimed at reproducing this family and at analyzing the differences in the outcome between those two models. Our results show that a reasonable match to the estimated size distribution of the real family is produced from the disruption of a porous parent body by the head-on impact of a projectile 54 km in size at 3 km s^(-1). Thus, our simulations with a model consistent with the assumed dark type of the family requires a smaller projectile than previously estimated, but the difference remains small enough to not affect the proposed scenario of this family history. We then find that the break-up of a porous body leads to different outcomes than the disruption of a non-porous one. The real properties of the Baptistina family still contain large uncertainties, and it remains possible that its formation did not involve the proposed impact conditions. However, the simulations presented here already show some range of outcomes and once the real properties are better constrained, it will be easy to check whether one of them provides a good match.
    Type
    Article
    text
    Language
    en
    ISSN
    1945-5100
    ae974a485f413a2113503eed53cd6c53
    10.1111/j.1945-5100.2009.tb01997.x
    Scopus Count
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    Meteoritics & Planetary Science, Volume 44, Number 12 (2009)

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