| Titre | The effects of crater degradation and target differences on the morphologies of Martian complex craters |
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| Auteur | Whitehead, J; Grieve, R A F; Garvin, J B; Spray, J G |
| Source | Large meteorite impacts and planetary evolution IV; par Reimold, W U (éd.); Gibson, R L (éd.); Geological Society of America, Special Paper no. 465, 2010 p. 67-80, https://doi.org/10.1130/2010.2465(05) |
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| Année | 2010 |
| Séries alt. | Secteur des sciences de la Terre, Contribution externe 20080729 |
| Éditeur | Geological Society of America |
| Document | publication en série |
| Lang. | anglais |
| DOI | https://doi.org/10.1130/2010.2465(05) |
| Media | papier; en ligne; numérique |
| Formats | pdf |
| Région | Mars |
| Sujets | cratères; cratères météoriques; morphologie; géologie extraterrestre |
| Illustrations | images; graphiques; histogrammes; tableaux |
| Diffusé | 2010 11 24 |
| Résumé | (disponible en anglais seulement)
We compared the target types and the morphologies and morphometries of various features within fresh complex craters on Mars to assess target dependence. The
wide scatter in depth-diameter data from Martian craters is more pronounced than for lunar or Mercurian craters. This was previously assumed to be predominantly due to significant degrees of denudation and secondary infilling of the Martian craters.
However, our data for fresh craters still exhibit a wide variation, which we interpret to be the result of comparatively higher target heterogeneity on Mars. Complex central peaks exhibit some crater diameter dependence: preferentially occurring in
craters >50 km. Neither peak complexity nor geometry show any statistical correlations with target type. Although central peak uplift heights and aspect ratios do not exhibit any clear target dependence, they do appear to be correlated, with higher
peaks possessing narrower aspect ratios.
Floor and summit pits appear to be more common on lava targets than sedimentary targets, contrary to earlier studies with smaller sample sizes. This observation imposes additional constraints on models
proposed for the origin of pits, especially those models that require the presence of volatiles in the target.
The ability to correlate target type with crater morphologies/morphometries is highly contingent upon both the surface geology, and the
actual geology at depth. Some weak correlations may reflect our current limited understanding of sub-surface geology on Mars. Information on the deeper lithologies acquired through future missions may help resolve the true effect of sub-surface
competence on intracrater structure. |
| GEOSCAN ID | 226640 |
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