ABSTRACT The Popigai (100 km in diameter) and the Chesapeake Bay (40–85 km diameter) impact structures formed within ~10–20 k.y. in the late Eocene during a 2 m.y. period with enhanced flux of 3 He-rich interplanetary dust to Earth. Ejecta from the Siberian Popigai impact structure have been found in late Eocene marine sediments at numerous deep-sea drilling sites around the globe and also in a few marine sections outcropped on land, like the Massignano section near Ancona in Italy. In the Massignano section, the Popigai layer is associated with an iridium anomaly, shocked quartz, and abundant clinopyroxene-bearing (cpx) spherules, altered to smectite and flattened to “pancake spherules.” The ejecta are also associated with a significant enrichment of H-chondritic chromite grains (>63 μm), likely representing unmelted fragments of the impactor. The Massignano section also contains abundant terrestrial chrome-spinel grains, making reconstructions of the micrometeorite flux very difficult. We therefore searched for an alternative section that would be more useful for these types of studies. Here, we report the discovery of such a section, and also the first discovery of the Popigai ejecta in another locality in Italy, the Monte Vaccaro section, 90 km west of Ancona. The Monte Vaccaro section biostratigraphy was established based on calcareous nannoplankton, which allowed the identification of a sequence of distinct bioevents showing a good correlation with the Massignano section. In both the Monte Vaccaro and Massignano sections, the Popigai ejecta layer occurs in calcareous nannofossil zone CNE 19. The ejecta layer in the Monte Vaccaro section contains shocked quartz, abundant pancake spherules, and an iridium anomaly of 700 ppt, which is three times higher than the peak Ir measured in the ejecta layer at Massignano. In a 105-kg-size sample from just above the ejecta layer at Monte Vaccaro, we also found an enrichment of H-chondritic chromite grains. Because of its condensed nature and low content of terrestrial spinel grains, the Monte Vaccaro section holds great potential for reconstructions of the micrometeorite flux to Earth during the late Eocene using spinels.

ABSTRACT The present-day ocean-climate system configuration took shape during the Miocene Epoch. Toward the end of the epoch, in the late Tortonian at ca. 8.5 Ma, there was an exceptional event: collisional disruption of an >150-km-diameter asteroid, which created the Veritas family of asteroids in the asteroid belt. This event increased the flux of interplanetary dust particles rich in 3 He to Earth and probably caused a period of increased dust in the atmosphere, with consequent alteration of global and local environmental conditions. A late Miocene 3 He anomaly likely related to the Veritas event has been registered in deep-sea sediments from Ocean Drilling Program (ODP) Site 926 (Atlantic Ocean), ODP Site 757 (Indian Ocean), and in the late Tortonian–early Messinian Monte dei Corvi section near Ancona, Italy. Here, we report the results of a study in the Monte dei Corvi section aimed to recover extraterrestrial chrome-spinel grains across the 3 He anomaly interval, as has been done for the similar late Eocene 3 He anomaly in the nearby Massignano section. In this study, three ~100 kg samples were collected from the Monte dei Corvi section: two within the 3 He peak interval and one outside the anomaly interval as a background reference sample. In total, 1151 chrome-spinel grains (>63 µm) were recovered, but based on chemical composition, none of the grains has a clear extraterrestrial origin. This supports the inference that the 3 He anomaly is indeed related to the Veritas event and not to an approximately coeval breakup of a smaller H-chondritic body in the asteroid belt, an event registered in meteoritic cosmic-ray exposure ages. Spectral studies of the Veritas asteroids indicate that they are made up of carbonaceous chondritic material. Such meteorites generally have very low chrome-spinel concentrations in the grain-size range considered here, contrary to the very chromite-rich ordinary chondrites. The terrestrial grains recovered were classified, and their composition showed that all the grains have an ophiolitic origin with no substantial compositional and distributional change through the section. The source area of the terrestrial grains was probably the Dinarides orogen.

ABSTRACT Two late Eocene impact spherule layers are known: the North America microtektite layer (from the Chesapeake Bay crater) and the slightly older clinopyroxene (cpx) spherule layer (from Popigai crater). Positive Ir anomalies occur at 5.61 m and 6.19 m above the base of a late Eocene section at Massignano, Italy. The age difference between the two anomalies is ~65 ± 20 k.y. The older Ir anomaly at 5.61 m appears to be associated with the cpx spherule layer. Although no impact spherules or shocked-mineral grains have been found associated with the upper Ir anomaly at 6.19 m, it has been proposed that it may be from the Chesapeake Bay impact. Comparison with other distal ejecta layers suggests that microtektites, but not shocked-mineral grains, from the Chesapeake Bay crater could have been thrown as far as Massignano. However, their absence neither supports nor disproves the hypothesis that the Ir anomaly at 6.19 m is from the Chesapeake Bay impact. On the other hand, the North American microtektite layer is not associated with an Ir anomaly. Furthermore, the average age difference between the cpx spherule layer and the North American microtektite layer appears to be ~18 ± 11 k.y., which is nearly one quarter the age difference between the two Ir anomalies at Massignano. This indicates that the Ir anomaly at 6.19 m is too young to be from the Chesapeake Bay impact, and thus is most likely not from the Chesapeake Bay impact.

ABSTRACT The late Eocene was marked by multiple impact events, possibly related to a comet or asteroid shower. Marine sediments worldwide contain evidence for at least two closely spaced impactoclastic layers. The upper layer might be correlated with the North American tektite-strewn field (with the 85-km-diameter Chesapeake Bay impact structure [USA] as its source crater), although this is debated, whereas the lower, microkrystite layer (with clinopyroxene [cpx]-bearing spherules) was most likely derived from the 100-km-diameter Popigai impact crater (Russia). The Eocene-Oligocene global stratotype section and point is located at Massignano, Italy, and below the boundary, in the late Eocene, at the 5.61 m level, shocked quartz and pancake-shaped smectite spherules that contain (Ni- and Cr-rich) magnesioferrite spinel crystals are found. These are associated with a positive Ir anomaly in deposits with the same age as the Popigai-derived cpx spherule layer. This layer is overlain by another Ir-rich layer, likely due to another large impact event. From a large amount of “pancake-bearing” rock, we isolated a few hundred milligrams of this spinel-rich material. The tungsten isotopic composition of this material shows more or less a terrestrial composition. However, the spinel-rich materials have excess 54 Cr values (expressed as ε 54 Cr, which is the per ten thousand deviation of the 54 Cr/ 52 Cr ratio from a terrestrial standard) of around –0.4 to –0.5 ε 54 Cr, which distinctly point to an ordinary chondritic impactor. This result supports the asteroid impact interpretation but not the comet impact hypothesis.

The Ancona Penrose Conference of October 2007 dealt with the current state of understanding of the late Eocene and the Eocene-Oligocene boundary, ~34 million years ago, a critical but very brief interval in Earth history. In this paper, we place that brief interval and the lessons from the conference in the broadest possible context by viewing them in the light of “Big History.” This new intellectual concept maintains that there may be value in considering the entire past, from the big bang until today, as a single unit of study. At this very early stage in the study of Big History, not even the most fundamental questions have been well formulated, let alone answered. As a first cut, Big History can be divided into regimes by considering the disciplines that study it: cosmic history (studied by cosmology and astronomy), Earth history (studied by geology), life history (studied by paleontology and evolutionary biology), and human history (studied by archaeology and historiography). These disciplines differ in terms of problems, techniques, and intellectual traditions. If we seek a common basis for a finer subdivision, the changes in utilization of the energy that have driven historical changes would seem like a good candidate. In two thought-provoking papers in 2007, Robert Aunger proposed “periodizing” all of history by placing divisions between periods when new methods of utilizing concentrated energy came into being, e.g., cellular metabolism or human agriculture. Aunger draws a parallel between this periodization of Big History and the establishment of the geological time scale. In this paper, we carefully consider this parallel and conclude that periodizing history on the basis of energy use or any other conceptual scheme is quite different from the division of Earth history into the intervals that yielded the geological time scale. Both are important but they have different purposes. Time-scale construction is a procedure that ties history to the rocks that record the history. It is a necessary step in reconstructing Earth and life history but is neither necessary nor possible in studying the history of cosmos or humanity. In contrast, periodizing history into intervals provides a conceptual framework on which to hang a growing understanding of history. We conclude that it is important to differentiate between (1) time-scale construction, (2) correlating events, (3) dating events, and (4) periodizing history. In this light, Aunger’s focus on changes in energy use remains an instructive way of periodizing history, but it must be clearly differentiated from time-scale construction.

The late Eocene may have been a period with an enhanced flux of extraterrestrial matter to Earth related either to a comet or an asteroid shower. The evidence comes from two very large and several medium-sized impact craters, at least two microtektite-microkrystite layers, and a stratigraphic interval with enhanced extraterrestrial 3 He, all within the period ca. 36.3–34.3 Ma. Here, we show that the distribution of sediment-dispersed extraterrestrial (ordinary chondritic) chromite (EC) grains in the Massignano section, central Italy, can be used to test whether the flux of ordinary chondritic matter to Earth was enhanced in the late Eocene. In twelve limestone samples, each weighing ~12–15 kg, from 1.25 m to 10.25 m above the base of the section, only 1 EC grain was found. Based on the total amount of limestone analyzed, 167 kg, this corresponds to 0.006 EC grain kg ‒1 limestone. This is a factor of five lower than the 0.029 EC grain kg ‒1 recovered in 210 kg of latest Cretaceous–Paleocene limestone from the Bottaccione Gorge section at Gubbio, central Italy. The difference can readily be explained by an approximately threefold higher sedimentation rate in the late Eocene at Massignano. In essence, our results speak against a late Eocene asteroid shower. Apparently, there was no significant increase in the flux of extraterrestrial chromite at this time, such as that after the disruption of the L-chondrite parent body in the mid-Ordovician, when the EC flux was enhanced by two orders of magnitude. We also discuss the potential to search for lunar minerals in the Massignano section in order to test the recent hypothesis that late Eocene 3 He enrichments originated from impact-ejected lunar regolith.

The Eocene-Oligocene transition marks the passage from “greenhouse” conditions to an “icehouse state” with progressive global cooling starting in the early middle Eocene. The late Eocene is also characterized by a high concentration of extraterrestrial impacts, the effects of which, on living organisms and climatic changes, are still not understood. We carried out a high-resolution investigation on planktonic foraminiferal assemblages in an 8-m-thick segment of the Massignano global stratotype section and point for the Eocene-Oligocene boundary with the aim of assessing the effects that the impacts may have had on the environment and this group of organisms. The studied interval is punctuated by three late Eocene iridium-rich layers, several cosmic signatures, and enhanced levels of 3 He. The two lower closely spaced iridium anomalies are possibly linked to the Popigai and Chesapeake Bay impact events, respectively, whereas no particular impact event can be assigned to the third anomaly, even if it might be correlated with some large craters. Interpretation of data suggests that all the impacts had no abrupt, dramatic effects on planktonic foraminifera. However, acting as forcing factors, they induced some environmental perturbations and may have contributed to remarkable climate changes superimposed on the general late Eocene cooling trend. The Popigai and Chesapeake Bay impact events triggered significant changes in the water mass structure, in terms of stratification and trophic resources, associated with some climatic excursions that took place within chron C16n.1n and chron C15r and at the transition between planktonic foraminiferal zones P15 and P16. The short-term warming pulse recognized after the Popigai impact might have been due to greenhouse effects produced by injection of CO 2 into the atmosphere and/or the release of methane hydrate after the impact itself. The dynamic between hydrological and climate changes across the impactoclastic layers as observed at Massignano displays different features at each impact event, probably due to the context in which each occurred in terms of impactor size, location, and target rocks. The relatively long duration of the enhanced cooling following the Chesapeake Bay impact suggests that this event induced a progressive cooling and triggered a feedback mechanism that sustained the initial impact-induced changes. Similar patterns of climatic excursions reported worldwide across the equivalent impact-ejecta horizons indicate that the impact-induced climate changes recorded at Massignano appear to be global in extent.

High-resolution spectral analyses of four climate proxies from Massignano, Italy (Eocene-Oligocene boundary global stratotype section and point [GSSP]), indicate that the deposition of this rhythmically bedded sedimentary sequence was controlled by Milankovitch orbital cycles. An inverse relationship between the magnetic susceptibility record and the co-varied calcium carbonate, δ 18 O, and δ 13 C records is indicative of a climate model in which limestones represent dry/cold periods, while marly limestones represent warm/wet periods. Through pattern matching of band-pass filtered signals with the La2004 eccentricity curve, we propose an astrochronological calibration for this important time period. Constrained by three radioisotopically dated volcanic ashes and based on a band-pass version of eccentricity that exhibits expected amplitude modulations, our astrochronology yields a refined age for the Eocene-Oligocene boundary of 33.91 ± 0.05 Ma. Orbital forcing is less pronounced in the lower portion of the Massignano section (meter levels 0–15), which contains evidence of several impact events and a 2.2-m.y.-long comet/asteroid shower. We propose that substantial, nonperiodic climate alterations caused by this period of enhanced extraterrestrial activity mask the Milankovitch climate cycles. Possible mechanisms for the exaggeration of impact-related climatic changes include the ice-albedo feedback or the combined effect of impact-related atmospheric alterations with ongoing dust-particle loading associated with the comet/asteroid shower.

Published radioisotopic (K/Ar, 40 Ar/ 39 Ar, and Rb/Sr) and astronomical ages for the Eocene-Oligocene boundary are essentially consistent at ca. 33.8 ± 0.1 Ma, but the 40 Ar/ 39 Ar ages have been calculated relative to an outdated age of 27.83–27.84 Ma for the Fish Canyon Tuff sanidine dating standard. Application of a revised age of 28.02 Ma, or the new astronomically calibrated age of 28.201 Ma, leads to significant discrepancies, while others are eliminated. In particular, the astronomically tuned ages of ca. 33.79 Ma at Ocean Drilling Program (ODP) Site 1218 and of 33.90–33.95 Ma at Massignano–Monte Cagnero are now in good agreement with recalculated (alternative) 40 Ar/ 39 Ar sanidine ages for the boundary as derived from the volcanic ignimbrite complex in New Mexico and for the Persistent White Layer (PWL) ash bed in North America, which is supposed to closely correspond to the boundary. This mutual consistency suggests that the tuning is correct at the scale of the 400 k.y. eccentricity cycle. Evidently, additional single-crystal 40 Ar/ 39 Ar sanidine dates from the tuffs in North America and independent checks on the astronomical tuning and the intercalibration between the astronomical and 40 Ar/ 39 Ar dating methods are needed to definitively solve the problem of the numerical age of the Eocene-Oligocene boundary. It is anticipated that such analyses and tests will be carried in the coming years as part of the international Earthtime initiative and associated projects to significantly improve the geological time scale. Clearly, an accurate and precise dating of the Eocene-Oligocene boundary is crucial if we are to unravel the underlying cause of the major climate transition associated with it.

The interval from the middle Eocene to early Oligocene represents one of the most significant transitions in Earth’s climate, during which greenhouse conditions were supplanted by icehouse conditions of the present day. This global transition was preceded by a long-term cooling phase and short-term uncorrelated variations in several marine proxies, which indicate paleoceanographic instabilities prior to the key climatic transition. We integrate previous multidisciplinary studies with recent data from the Massignano section (Umbria-Marche Basin) and summarize interpretations of studies from the past 20 yr that have been based on the Eocene-Oligocene boundary global stratotype section and point (GSSP). Based on the many data sets from this section, with an emphasis on the rock magnetic data, we propose that the fluctuations and final cessation of a westward subtropical Eocene Neotethys (STENT) current were drivers in the climatic transition from greenhouse to icehouse conditions. Our hypothesis considers that the global variable climatic conditions were synchronous to large changes in circulation in the western Neotethys Ocean, which were primarily due to paleogeographic and sea-level changes. Specifically, the closing of the gateway between the Arabian and Eurasian plates, through coupling of sea-level changes, could represent the threshold or one of the triggers that caused the paleoceanographic variations in the Neotethys and in global ocean circulation patterns during the end of the Eocene.

We present the results of integrated biostratigraphic (planktonic foraminifera, calcareous nannofossils, and dinoflagellates), magnetostratigraphic, and cyclostratigraphic analyses of the lower part of Monte Cagnero section (Umbria-Marche Apennines of Italy), a continuous and complete succession of pelagic limestone and marls that provides the means for an accurate and precise astrochronologic calibration of the Eocene-Oligocene transition. This 38.5-m-thick section overlaps the Oligocene section, which, at meter level 188, contains the Rupelian-Chattian boundary corresponding to the O4-O5 planktonic foraminiferal zonal boundary within the upper half of magnetochron C10n. The Eocene-Oligocene boundary at Monte Cagnero, as defined by the last occurrence of hantkeninid planktonic foraminifers (E14-E15 zonal boundary), is found at meter level 114.1, in the upper part of calcareous nannofossil zone CP16a, and very near the Aal-Gse dinocyst zonal boundary. Paleomagnetic analysis has identified all the magnetic reversals from the lower C13r to the lower C12n, precisely overlapping the base of the Oligocene magnetostratigraphic succession and placing the Eocene-Oligocene boundary in the upper part of C13r, in full agreement with the global stratotype section and point (GSSP) at Massignano. Spectral analysis of calcium carbonate data from bulk samples, collected at 5 cm intervals, indicates that orbital forcing of depositional cycles (i.e., limestone versus marl alternations) is dominant at frequencies corresponding to the theoretical astronomical curves of eccentricity, obliquity, and precessional cycles throughout the studied Eocene-Oligocene transition. Correlation with the astrochronologic time scale allows an age assignment of 33.95 Ma for the Eocene-Oligocene boundary, which is in close agreement with the astrochronologic age for the boundary in the GSSP of Massignano obtained in a similar study by R.E. Brown and colleagues in this volume. Thus, the Monte Cagnero section represents a candidate parastratotype for the Eocene-Oligocene GSSP of Massignano in the eventuality that the oxygen and carbon stable isotope shifts defining the oxygen isotope Oi-1 glaciation will be preferred over the last occurrence of hantkeninids as marker for the boundary, since, at Massignano, the beginning of this isotope shift is barely represented in the uppermost part of the exposed section. The excellent integrated stratigraphic framework of Monte Cagnero presented here will significantly facilitate further high-resolution isotope and paleoecological studies across the time of transition from a hothouse to icehouse Earth.