A complete and easily accessible means of calculating surface exposure ages or erosion rates from Be and Al measurements

We codify previously published means of calculating exposure ages and erosion rates from ¹⁰Be and ²⁶Al concentrations in rock surfaces, and present a single complete and straightforward method that reflects currently accepted practices and is consistent with existing production rate calibration measurements. It is intended to enable geoscientists, who wish to use cosmogenic-nuclide exposure age or erosion rate measurements in their work to: (a) calculate exposure ages and erosion rates; (b) compare previously published exposure ages or erosion rate measurements on a common basis; (c) evaluate the sensitivity of their results to differences between published production rate scaling schemes. The method is available online at http://hess.ess.washington.edu.     

The pedigree and influence of fossil collections from the Falkland Islands: From Charles Darwin to continental drift

The Falkland Islands are typical of remote territories in that their early geological exploration was piecemeal and opportunistic. Whilst the resulting fossil collections (dominantly a Devonian fauna of the Malvinokaffric realm) remain the basis for modern interpretations, published accounts misrepresent their extent and provenance. Charles Darwin first discovered fossils during his 1833 visit aboard HMS Beagle, with subsequent British collections acquired in 1842 and 1876, respectively, by the Erebus and Terror and Challenger expeditions and in 1903 by the Scotia expedition. Darwin's collection, and much of the other material, is now held by The Natural History Museum, London (NHM) but some Darwin specimens were assimilated into other collections whilst at least one NHM ‘Darwin’ specimen was not collected by him. There may also be some uncertainty as to the origin of the Scotia collection, now held in Edinburgh by National Museums Scotland, in relation to a contemporary Swedish collection now held in Stockholm. The NHM holdings were supplemented by a number of enigmatic donations from private individuals and then by fossils collected during the first ‘official’ geological survey of the islands in 1920–1922. Meanwhile a large collection was built up in New York through collaboration in 1909 with a local collector – the Governor's wife! The regional associations of the fossils established the African heritage of Falklands geology, and thereby contributed to an understanding of continental drift as the mechanism for the fragmentation of the Gondwana supercontinent. The Falkland Islands are now regarded as a rotated microplate created during the break-up.     

Hydromagmatic amphibole in komatiitic, tholeiitic and ferropicritic units, Abitibi greenstone belt, Ontario and Québec: evidence for Archaean wet basic and ultrabasic melts

Summary ?Detailed petrographic, electron microprobe and ion probe studies of Archaean hydromagmatic amphiboles from the Abitibi greenstone belt, Canada, yield new insights into the origin of Al-undepleted komatiitic and Al-depleted tholeiitic and ferropicritic melts. The amphiboles are present in peridotite layers and basal chill zones of thick differentiated basic and ultrabasic sills and flows, and are titanian pargasite–hastingsite in composition. They can be grouped into two petrographic types: (1) amphibole in the groundmass; and (2) amphibole-bearing melt inclusions. The groundmass amphiboles are oikocrysts, rims and interstitial grains, present in minor to major amounts. The oikocrysts host cumulus olivines (Fo_83–84) that are rounded in shape, embayed, and smaller in size. The amphibole-bearing melt inclusions are hosted in cumulus olivines (Fo_83–84 in komatiitic rocks and Fo₇₉ in tholeiitic rocks), spherical to ovoid in shape, 50–500 μm in size, and dominated modally by amphibole. The melt inclusions also contain euhedral chromite and aluminous spinel and micrometric clinopyroxene and glass, and sub-micrometric iron–nickel sulphide, chloro-apatite and ilmenite. In-situ ion probe analyses indicate the amphibole is: (1) enriched in Nb, LREE and Zr and depleted in Sr and HREE relative to primitive mantle; (2) contains up to 1–3 wt% H₂O; and (3) overall displays δD values from 50‰ to −140‰, including many values in the accepted magmatic range of −60‰ to −90‰. The petrographic relationships and geochemical compositions, and comparisons to experimental systems, indicate amphibole formation by subsolidus reaction of residual hydrous silicate melt with olivine and clinopyroxene. Some of the hydrous melt intruded and was entrapped as secondary melt inclusions within relict olivine. Rapid crystallization of the hydrous melt inclusions formed amphibole+clinopyroxene±glass±spinel or solely glass. Bulk compositions of the melt inclusions, comparisons to experimental phase equilibria, and presence of magmatic water suggest amphibole crystallisation from olivine → pyroxene residual melts with at least 2–3 wt% H₂O during rapid solidification of the host units. Adjustment for anhydrous phase crystallization (mainly olivine) suggests the initial melts contained 1–2 wt% H₂O. Such high H₂O contents and the magmatic δD compositions are consistent with the participation of H₂O in melt petrogenesis. However, most Abitibi komatiites and tholeiites lack hydromagmatic minerals, making it difficult to attribute all basic and ultrabasic melts to melting in hydrous Archaean mantle. The favoured model is that some Abitibi basic and ultrabasic melts were wet and some were dry, as well as Al-depleted or Al-undepleted. Received July 24, 2001; revised version accepted January 9, 2002     

> 25 MeV Proton Events Observed by the High Energy Telescopes on the STEREO A and B Spacecraft and/or at Earth During the First ∼ Seven Years of the STEREO Mission

Using observations from the High Energy Telescopes (HETs) on the STEREO A and B spacecraft and similar observations from near-Earth spacecraft, we summarize the properties of more than 200 individual >?25 MeV solar proton events, some detected by multiple spacecraft, that occurred from the beginning of the STEREO mission in October 2006 to December 2013, and provide a catalog of these events and their solar sources and associations. Longitudinal dependencies of the electron and proton peak intensities and delays to onset and peak intensity relative to the solar event have been examined for 25 three-spacecraft particle events. Expressed as Gaussians, peak intensities fall off with longitude with σ=47±14^° for 0.7?–?4 MeV electrons, and σ=43±13^° for 14?–?24 MeV protons. Several particle events are discussed in more detail, including one on 3 November 2011, in which ～?25 MeV protons filled the inner heliosphere within 90 minutes of the solar event, and another on 7 March 2012, in which we demonstrate that the first of two coronal mass ejections that erupted from an active region within ～?1 hour was associated with particle acceleration. Comparing the current Solar Cycle 24 with the previous cycle, the first >?25 MeV proton event was detected at Earth in the current solar cycle around one year after smoothed sunspot minimum, compared with a delay of only two months in Cycle 23. Otherwise, solar energetic particle event occurrence rates were reasonably similar during the rising phases of Cycles 23 and 24. However, the rate declined in 2013, reflecting the decline in sunspot number since the peak in the northern-hemisphere sunspot number in November 2011. Observations in late 2013 suggest that the rate may be rising again in association with an increase in the southern sunspot number.