Thematic Articles

Salt as a Host Rock for the Geological Repository for Nuclear Waste

Rock salt formations can make suitable hosts for the disposal of high-level radioactive wastes. The performance of salt as a host rock for a repository over million-year timescales has been investigated for the potential site for a geological repository at Gorleben in Germany. The main threat towards the stability of a natural salt barrier is its high solubility. Hence, prevention of water access into the waste emplacement area has to be ensured. Geological factors to be assessed in this context include diapirism, the formation of (future) glacial channels, the impact of loads and stresses imposed by glaciers, hydrocarbons, and the local hydrogeology. The disadvantages of salt are, however, outweighed by its beneficial properties: high thermal conductivity, good hydro-mechanical properties, and a tendency to creep and thus seal cracks. These characteristics make rock salt a very attractive candidate to host a geological repository for essentially all kinds of radioactive waste.

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The Russian Strategy of using Crystalline Rock as a Repository for Nuclear Waste

The first Russian underground repository for high- and intermediate-level radioactive waste (HLW and ILW, respectively) will be built in the crystalline Archean granite–gneisses at Yeniseisky (Krasnoyarsk region, Siberia). The geological and hydrogeological characteristics of this site are similar to those found in Forsmark (Sweden) and Olkiluoto (Finland). However, the Russian disposal strategy is different. HLW will be disposed in the form of an aluminophos­phate glass and ILW (with long-lived radionuclides) will be cemented. Preliminary research on all aspects of repository design (stability of waste forms, waste packages, and bentonite buffer; evaluation of the geologic barrier; and simulation of radionuclide transport by groundwater) will be performed at an on-site underground research laboratory.

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Crystalline Rock as a Repository for Swedish Spent Nuclear Fuel

The granitic bedrock at Forsmark (Sweden) provides a well suited host rock for a geological repository in which to safely dispose of spent nuclear fuel. The properties of the host rock have been thoroughly investigated through boreholes from the surface. This repository will be at a depth of approximately 500 m where the spent nuclear fuel will be contained in 6,000 copper canisters able to withstand potential earthquakes and glaciation events. The canisters will be surrounded by a bentonite clay buffer to prevent canister corrosion by groundwater. The safety assessment in support of the site’s license application suggests that almost all of the canisters will remain tight even one million years into the future.

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Geological Disposal of Radioactive Waste in Clay

Keeping future generations safe from today’s nuclear waste relies on this waste being effectively isolated for all time. Clay rocks, or rocks with a high clay content, offer promising isolation properties over time periods that are as long as the age of their host geological formations. Constructing a repository in such material does not significantly change the clay’s isolation properties, which is a great advantage. Isolation is a function of the interplay between the slow release of radionuclides from the waste, the diffusion-controlled radionuclide migration, the establishment of a reducing geochemical environment, and the weak solubility and strong retention of the most toxic radionuclides on clay minerals and on additional engineered barrier materials.

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Geological Disposal of Nuclear Waste: a Primer

The back-end of the nuclear fuel cycle has become the Achilles Heel of nuclear power. After more than 50 years of effort, there are, at present, no operating nuclear waste repositories for the spent nuclear fuel from commercial nuclear power plants or for the high-level waste from the reprocessing of spent fuel. The articles in this issue of Elements describe the status of geological disposal in salt, crystalline rock, clay, and tuff, as presently developed in five countries.

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Cosmic Dust Toolbox: Microanalytical Instruments and Methods

When cosmic dust particles were first identified almost 140 years ago, few would have predicted that much would ever be known about these miniscule objects, given the existing state of the art in analytical techniques. Times have changed. Today, in a single extraterrestrial dust particle, we can detect all the elements present, measure isotopic ratios, determine the exact crystalline structures of the minerals and the oxidation state of cations in those minerals, and even resolve individual atoms. The results are telling fascinating stories about the nature and histories of the particles that come to Earth. We review the most common techniques that help unravel these cosmic stories.

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Geochemical Tracers of Extraterrestrial Matter in Sediments

Every year, tens of thousands of tons of cosmic dust accumulate at the Earth’s surface, representing a continuation of the accretion process that started 4.57 billion years ago. The unique geochemical properties of these materials, compared to the Earth’s surface, render them excellent tracers of Solar System, atmospheric, oceanographic, and geologic processes. These processes can be recovered from the records preserved in marine and terrestrial sediments, including snow and ice. We review evidence from these natural archives to illuminate temporal and spatial variations in the flux and composition of extraterrestrial material to Earth, as well as the terrestrial processes that affect the distribution of extraterrestrial tracers in sediments.

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Organic Matter in Cosmic Dust

Organics are a significant component of most cosmic dust, as revealed from actual samples of extraterrestrial dust in the Earth’s stratosphere, in Antarctic ice and snow, in near-Earth orbit, and in asteroids and comets. Cosmic dust contains a diverse population of organic materials that owe their origins to a variety of chemical processes occurring in many different environments. The presence of isotopic enrichments of D and 15N suggests that many of these organic materials have an interstellar or protosolar heritage. The study of these samples is of considerable importance because they are the best preserved materials of the early Solar System available.

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Composition of Cosmic Dust: Sources and Implications for the Early Solar System

Many cosmic dust particles have escaped the aqueous and thermal processing, the gravitational compaction, and the impact shocks that often overprint the record, in most larger samples, of how Solar System materials formed. The least-altered types of cosmic dust can, therefore, act as probes into the conditions of the solar protoplanetary disk when the first solids formed. Analyses of these “primitive” particles indicate that the protoplanetary disk was well mixed, that it contained submicron grains formed in a diversity of environments, that these grains were aerodynamically transported prior to aggregation, which was likely aided by organic grain coatings, and that some minerals that condensed directly from the disk are not found in other materials. These protoplanetary aggregates are not represented in any type of meteorite or terrestrial rock. They can only be studied from cosmic dust.

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Cosmic Dust: Finding a Needle in a Haystack

Collecting cosmic dust is a tricky business! Despite Earth’s surface being showered by thousands of tons of comic dust every year, such dust is quickly lost in a sea of terrestrial particles. Finding the tiny cosmic treasures requires collecting dust from the cleanest environments where the terrestrial particle background is low. The stratosphere can be sampled via high-flying aircraft, whereas sampling cosmic dust from polar regions and the deep sea requires techniques that concentrate the particles. Collection efforts are worth it. Cosmic dust derives from every dust-producing object in the Solar System, including ancient Solar System materials, possibly even interstellar materials, of a type not found in meteorites.

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