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On the Chronostratigraphy of Planetary Satellites and Asteroids On the Chronostratigraphy of Planetary Satellites and Asteroids Absolute Surface Age Determination of Small Planetary Bodies: Scaling the Lunar Crater Chronology System vorgelegt von Dipl.‐Geol. Nico Schmedemann Fachbereich Geowissenschaften Freie Universität Berlin Dissertation zur Erlangung des Grades Doktor der Naturwissenschaften (Dr. rer. nat.) Berlin, im Juli 2015 Hauptgutachter: Prof. Dr. R. Jaumann Freie Universität Berlin Institut für Geologische Wissenschaften Fachrichtung Planetologie und Fernerkundung und Deutsches Zentrum für Luft- und Raumfahrt Institut für Planetenforschung, Abt. Planetengeologie Zweitgutachter: Prof. Dr. S. v. Gasselt Freie Universität Berlin Institut für Geologische Wissenschaften Fachrichtung Planetologie und Fernerkundung Tag der Disputation: 1. Dezember 2015 Eidesstattliche Erklärung Hiermit versichere ich, die vorliegende Arbeit selbstständig angefertigt und keine anderen als die angegebenen Quellen und Hilfsmittel benutzt zu haben. Berlin, 2015 Danksagung Großer Dank gebührt dem zwischenzeitlich leider verstorbenen Herrn Prof. Dr. Gerhard Neukum (FU-Berlin) für die Vergabe des Themas und der damit verbundenen Einstellung als Wissenschaftlicher Mitarbeiter in der Fachrichtung Planetologie an der Freien Universität Berlin. Durch seine Beteiligung an zahlreichen aktiven Raumfahrtmissionen ergab sich für mich die Möglichkeit mit bisher unveröffentlichten Daten in den Projekten Cassini und Dawn zu arbeiten. Er hat mich oft dazu ermuntert neue Ideen im Detail an den vorhandenen Daten zu testen, mit früheren Ergebnissen zu vergleichen und dabei das große Bild nicht aus den Augen zu verlieren. Er bestand zudem auch auf starke Präsenz bei internationalen Konferenzen, die einen angeregten Gedankenaustausch mit anderen Fachkollegen ermöglichten, die oft auch grundsätzlich andere Ansichten vertreten haben. Da Herr Prof. Dr. Neukum meine Arbeit nicht mehr betreuen kann, möchte ich mich bei Herrn Prof. Dr. R. Jaumann (Deutsches Zentrum für Luft und Raumfahrt, FU- Berlin) dafür bedanken, dass er sich für meine Arbeit als Betreuer und Erstgutachter bereit erklärt hat. In seiner Funktion als „Head of the Geoscience Working Group“ im Dawnprojekt hatte er einen ganz besonderen Einblick in die Diskussionen rund um die Chronostratigrafie des Asteroiden Vesta, die ein wesentlicher Bestandteil dieser Arbeit ist. Weiterer Dank gebührt Herrn Prof. Dr. S. van Gasselt (FU-Berlin) für die Übernahme der Zweitbegutachtung dieser Arbeit. Ganz besonderer Dank gilt ihm außerdem für die sehr hilfreichen Hinweise zur Planung, zur Struktur und zum Erscheinungsbild der Arbeit. Als äußerst wertvoll empfand ich die langen und intensiven Diskussionen mit meinen Kollegen Dr. T. Kneissl, Dr. G. Michael und Dipl.-Geol. A. Neesemann über viele Details der Kraterverteilung und Chronologie auf Vesta aber auch über das eine oder andere Thema am Rande. Sehr hilfreiche Diskussionen schon zu Beginn meiner Arbeit bekam ich besonders von Dr. R. J. Wagner und Dipl.-Ing. T. Denk bezüglich des Cassini Projekts. Nicht vergessen möchte ich hierbei die Einführung in die Arbeit am Stereokomparator, die ich von Dr. S. C. Werner und Frau U. Wolf erhielt. Großer Dank für die Unterstützung in Fragen der Informationstechnologie gebührt Dipl.-Geol. S. H. G. Walter. Das betrifft nicht nur die Instandhaltung des Bürorech- ners, sondern die gesamte Infrastruktur in unserer Fachrichtung. Aufwendige Rechnungen und die Bilddatenprozessierung für diese Arbeit sind auch auf den Servern der Fachrichtung gelaufen. Ebenfalls bedanken möchte ich mich bei Dipl.- Ing. Heike Rosenberg für die Unterstützung in der Cassinibilddatenverwaltung und die liebevolle Ausrichtung der Weihnachtsfeiern bei der sie von weiteren Mitgliedern unserer Arbeitsgruppe unterstützt wurde. Insgesamt möchte ich mich vii bei der gesamten Arbeitsgruppe für die gute Zusammenarbeit und hilfsbereite Unterstützung bedanken. Die aktive Arbeit im Dawn Team hat mir zudem gezeigt, dass die richtige Erkenntnis oft nicht ein Resultat eines vorgegebenen Arbeitsablaufs ist, sondern das Ergebnis eines mitunter lebhaften Austauschs von wissenschaftlichen Argumenten, die dazu anhalten, noch genauer und noch akribischer zu arbeiten. Zum Abschluss gilt mein Dank auch meiner Familie und meinen Freunden, die immer fest an einen erfolgreichen Abschluss der Arbeit geglaubt haben. viii Abstract Based on recent geologic research it appears that meteoritc bombardment is a major agent in the exogenic dynamics of Earth and other planetary bodies, especially in more ancient times (e.g. Neukum, 1984; Hildebrand et al., 1991; Gehrels, 1995; Becker et al., 2004 and Bottke et al., 2012). Furthermore, meteoritic bombardment is one of the few foreseeable natural hazards which mankind is able to prepare for to a certain degree. This is true predominantly for larger projectiles which orbital characteristics is known well ahead of a potential impact. Predicting impact risks, however, requires a deep understanding of numerous processes, which eventually result in such an event. Even the simple comparison between the Moon and the Earth shows for instance, that the time-dependent behavior of the projectile flux as well as the crater size-frequency distribution, is hard to investigate thoroughly on Earth alone. This thesis aims to relate the understanding of the meteoritic bombardment in the Earth-Moon system to other dynamical regions of our Solar System. Resulting in a significant improvement in one of the key issues in the field of planetary sciences: the ability to date planetary surfaces from impact craters on bodies from the inner Solar System to the asteroid Main Belt and the giant planet satellites of the outer Solar System. This tool is key in understanding the geologic history of the investigated bodies since the terminal phase of planetary accretion about 4 Ga ago until today. The cratering records of planetary bodies and the related projectile dynamics in the inner Solar System are relatively well known from vast sets of remote sensing data of the Moon, Mars and to a lesser degree, Mercury. In the case of the Moon, absolute calibration of the measured crater frequencies was possible by radiometric dating of returned lunar rock and soil samples. For bodies in the asteroid Main Belt and beyond, in the outer Solar System, the smaller sets of remote sensing data, limitations in observations of projectiles, and incomplete models of projectile dynamics complicate the interpretation of the cratering records and thus the understanding of the geologic history of respective planetary bodies. The work presented in this thesis utilizes the lunar cratering record and adopts it with some customization for the investigated planetary bodies with significantly different impact environments than the Moon. By comparing the predictions of the lunar-like model and the observed cratering records at different locations in the Solar System (Martian satellite Phobos, Main Belt asteroids and Saturnian satellites) a significant increase in knowledge has been achieved about the projectiles’ origin and their dynamical characteristics. Applying the lunar-like cratering models to surface areas that are related to major geologic events on the investigated bodies allowed for the exploration of their individual geologic histories as well as, partially, their dynamical histories. A comparison of the geologic histories of the planetary bodies across the Solar System also offers a possibility to understand the development of the Solar System in many different aspects. Such aspects are for ix instance the projectile dynamics and collisional evolution of small bodies from the late stage planetary accretion until today. Stratigraphic relationships were used in order to test the lunar-like models and alternative models of other scientific working groups for consistency. Results from the Saturnian satellites Mimas and Iapetus, the Main Belt asteroids Vesta, Lutetia, Ida and Gaspra as well as the Martian satellite Phobos studied in this work showed that they are consistent with a lunar-like impact history. Under consideration of earlier work, the timing of youngest basin forming impact events on the Moon, Mars and the larger asteroids as well as the time of the Phobos capture and the catastrophic disruption of the precursor bodies of Ida and Lutetia lead to the conclusion of similar projectile flux characteristics at all of these bodies at the end of the heavy bombardment time period. During the first billion years of Solar System history the exponential decline in the Solar System-wide projectile flux could be interpreted as the tail of planetary accretion. In this respect the Saturnian system needs further analysis in order to find and properly date its youngest basin. For the Saturnian satellites Mimas and Iapetus the crater distributions suggest a planetocentric and collisionally evolved source of projectiles with relatively low impact velocities. Mimas appears to have been geologically inactive since its surface accumulated the currently observable craters. The satellite shows the same crater retention age (~4.3 Ga) over its whole surface. Its largest crater, Herschel, formed about 4 Ga ago. Crater size-distributions on the asteroids Ida, Gaspra, Lutetia and Vesta clearly show a lunar-like behavior that has previously been discussed and was expected to be shallower at small sizes based on modelling of collisional cascades of asteroids. In the case of the geologically complicated asteroid Vesta, absolute crater retention ages of basin forming events
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