Fundamental Research in High Energy Density Science (2023) / Chapter Skim
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broadening remote access to its major experimental and computing facilities. Leading Recommendation: To enhance career pathways for high energy density science research at NNSA facilities, the NNSA should (1)
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At these conditions, the forces between atoms, electrons, ions and even nucleons are profoundly modified, changing fundamental material properties, paving paths to the creation of entirely new forms of matter, and enabling conversion of matter into energy. Traditionally, the domain of HED science is defined by pressures exceeding 1 million times atmospheric pressure (see Figure 1-1)
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become frequent and violent enough that their nuclei begin to combine and react, leading to nuclear fusion. In HED science, "hot" is shorthand for the many kiloelectronvolts temperature that support nuclear fusion; "warm" indicates the many electronvolts (103-106 K)
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The trends of the Periodic Table of chemical elements are thus fundamentally transformed in the HED regime, with new materials, properties, and processes being observed. Hydrogen and helium, the most abundant chemical elements in the universe, trans form to fluid metals at HED conditions, for example, with liquid metallic hydrogen being the predominant constituent of stars and giant planets (see Figure 1-2)
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and for chemical-bond energies give an energy density of 1 eV/Å3 = 160 GPa, near the lower limit of HED conditions. Multiplying the HED onset (1011 J/m3)
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While the atomic-scale properties of materials at extreme conditions are fun damental to HED science, the behavior and performance of HED systems is often most relevant to applications. All HED experiments and astrophysical objects access an enormous range of materials, conditions, length scales, and time scales over the
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Ho, C Wild, et al., 2009, "Letter: Diamond Spheres for Inertial Confinement Fusion," Nuclear Fusion 49(11)
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Thus, it is not sufficient to understand the microphysics of HED science: we must also understand how samples interact with external fields; how inhomogeneous radiation distributions influence plasma evolution; and how instabilities form, grow, and evolve into turbulence and mix. This variety of phenomena -- from the quantum mechanics of chemical bond ing, to collective plasma effects, to strong coupling of matter with radiation, to thermonuclear processes, along with the enormous ranges of relevant length and time scales, from the atomic to the astrophysical -- leads to some of the fundamental excitement of HED science.
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In anticipation of continued advances in both computational and experimental capabilities, the committee prepared this report to assess the accomplishments, opportunities, and challenges of basic research in HED science. In addition, HED science has applications in core mission areas of the NNSA, including stewardship of the nation's nuclear weapons stockpile, countering pro liferation of the associated technologies, and development of nuclear fusion–based energy capabilities: areas in which the basic research described in the text by the BOX 1-3 The Language of High Energy Density Science Atomic pressures.
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High energy density matter. Matter at pressures above 1011 Joules/m3 = 100 GPa, conditions for which external forces begin to overwhelm chemical forces of ordinary matter on Earth.
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