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Stellarators. Present Status and Future Planning
STELLARATORS Present Status and Future Planning H. Wobig, Garching IMax-Planck-Institut für Plasmaphysikl magnetic axis Fig. 1 — Period of toroidally dosed magnetic surfaces. The stellarator is a closed toroidal device open-ended configurations like mirror ma designed to confine a hot plasma In a ma chines (see EN, 12 8/9) there are always gnetic field. It is one of the oldest concepts plasma particles which escape the confine magnetic surfaces is investigated by field to have been investigated in the search for ment volume along the magnetic field and line integration. The topology of the field controlled thermonuclear fusion. an isotropic distribution function cannot be lines is determined by the rotational trans The basic idea of the stellarator was maintained. If this anisotropy is too strong form or twist number 1/27t (or+), which is developed by Lyman Spitzer, Professor of it gives rise to instabilities and enhanced the number of revolutions of a field line Astronomy at Princeton in 19511). Experi plasma losses. It is mainly to avoid these around the magnetic axis during one toroi mental studies began in 1952 and after the disadvantages that toroidal confinement dal revolution. declassification of fusion research in 1958 has been preferred. The need for a helical field can be under the idea was picked up by other research In toroidal configurations, the currents stood from a look at the particle orbits. groups. In Europe, the first stellarators which generate the confining magnetic Charged particles tend to follow the field were built in the Max-Planck Institute for fields can be classified under three lines and unless these are helical, because Physics and Astrophysics in Munich and categories : of inhomogeneities, the particles will drift later at Culham, Moscow and Karkhov. -
L-Shell and Energy Dependence of Magnetic Mirror Point of Charged
Soni et al. Earth, Planets and Space (2020) 72:129 https://doi.org/10.1186/s40623-020-01264-5 FULL PAPER Open Access L-shell and energy dependence of magnetic mirror point of charged particles trapped in Earth’s magnetosphere Pankaj K. Soni* , Bharati Kakad and Amar Kakad Abstract In the Earth’s inner magnetosphere, there exist regions like plasmasphere, ring current, and radiation belts, where the population of charged particles trapped along the magnetic feld lines is more. These particles keep performing gyration, bounce and drift motions until they enter the loss cone and get precipitated to the neutral atmosphere. Theoretically, the mirror point latitude of a particle performing bounce motion is decided only by its equatorial pitch angle. This theoretical manifestation is based on the conservation of the frst adiabatic invariant, which assumes that the magnetic feld varies slowly relative to the gyro-period and gyro-radius. However, the efects of gyro-motion can- not be neglected when gyro-period and gyro-radius are large. In such a scenario, the theoretically estimated mirror point latitudes of electrons are likely to be in agreement with the actual trajectories due to their small gyro-radius. Nevertheless, for protons and other heavier charged particles like oxygen, the gyro-radius is relatively large, and the actual latitude of the mirror point may not be the same as estimated from the theory. In this context, we have carried out test particle simulations and found that the L-shell, energy, and gyro-phase of the particles do afect their mirror points. Our simulations demonstrate that the existing theoretical expression sometimes overestimates or underesti- mates the magnetic mirror point latitude depending on the value of L-shell, energy and gyro-phase due to underlying guiding centre approximation. -
Nicholas Christofilos and the Astron Project in America's Fusion Program
Elisheva Coleman May 4, 2004 Spring Junior Paper Advisor: Professor Mahoney Greek Fire: Nicholas Christofilos and the Astron Project in America’s Fusion Program This paper represents my own work in accordance with University regulations The author thanks the Program in Plasma Science and Technology and the Princeton Plasma Physics Laboratory for their support. Introduction The second largest building on the Lawrence Livermore National Laboratory’s campus today stands essentially abandoned, used as a warehouse for odds and ends. Concrete, starkly rectangular and nondescript, Building 431 was home for over a decade to the Astron machine, the testing device for a controlled fusion reactor scheme devised by a virtually unknown engineer-turned-physicist named Nicholas C. Christofilos. Building 431 was originally constructed in the late 1940s before the Lawrence laboratory even existed, for the Materials Testing Accelerator (MTA), the first experiment performed at the Livermore site.1 By the time the MTA was retired in 1955, the Livermore lab had grown up around it, a huge, nationally funded institution devoted to four projects: magnetic fusion, diagnostic weapon experiments, the design of thermonuclear weapons, and a basic physics program.2 When the MTA shut down, its building was turned over to the lab’s controlled fusion department. A number of fusion experiments were conducted within its walls, but from the early sixties onward Astron predominated, and in 1968 a major extension was added to the building to accommodate a revamped and enlarged Astron accelerator. As did much material within the national lab infrastructure, the building continued to be recycled. After Astron’s termination in 1973 the extension housed the Experimental Test Accelerator (ETA), a prototype for a huge linear induction accelerator, the type of accelerator first developed for Astron. -
Highlights in Early Stellarator Research at Princeton
J. Plasma Fusion Res. SERIES, Vol.1 (1998) 3-8 Highlights in Early Stellarator Research at Princeton STIX Thomas H. Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08540, USA (Received: 30 September 1997/Accepted: 22 October 1997) Abstract This paper presents an overview of the work on Stellarators in Princeton during the first fifteen years. Particular emphasis is given to the pioneering contributions of the late Lyman Spitzer, Jr. The concepts discussed will include equilibrium, stability, ohmic and radiofrequency plasma heating, plasma purity, and the problems associated with creating a full-scale fusion power plant. Brief descriptions are given of the early Princeton Stellarators: Model A, Model B, Model B-2, Model B-3, Models 8-64 and 8-65, and Model C, and also of the postulated fusion power plant, Model D. Keywords: Spitzer, Kruskal, stellarator, rotational transform, Bohm diffusion, ohmic heating, magnetic pumping, ion cyclotron resonance heating (ICRH), magnetic island, tokamak On March 31 of this year, at the age of 82, Lyman stellarator was brought to the headquarters of the U.S. Spitzer, Jr., a true pioneer in the fields of astrophysics Atomic Energy Commission in Washington where it re- and plasma physics, died. I wish to dedicate this presen- ceived a favorable reception. Spitzer chose the name tation to his memory. "Project Matterhorn" for the project which was to be Forty-six years ago, in early 1951, Spitzer, then sited in the Princeton area, on the newly acquired For- chair of the Department of Astronomy at Princeton restal tract, and funding began on July 1 of that year University, together with Princeton physicist John 121- Wheeler, had been thinking about the physics of ther- Spitzer's earliest stellarator papers comprise a truly monoclear processes. -
NONDIMENSIONAL TRANSPORT SCALING in Dlll-D: BOHM VERSUS GYRO-BOHM RESOLVED
GA-A21904 NONDIMENSIONAL TRANSPORT SCALING IN Dlll-D: BOHM VERSUS GYRO-BOHM RESOLVED by C.C. PETTY, T.C. LUCE, K.H. BURRELL, S.C. CHIU, J.S. deGRASSIE, C.B. FOREST, P. GOHIL, CM. GREENFIELD, R.J. GROEBNER, R.W. HARVEY, R.I. PINSKER, R. PRATER, R.E. WALTZ, R.A. JAMES,* and D. WROBLEWSKI* This is a preprint of an invited paper presented at the 1994 American Physical Society Division of Plasma Physics Meeting, November 7-11,1994, Minneapolis, Minnesota, and to be printed in the Proceedings. Work supported by U.S. Department of Energy under Contracts DE-AC03-89ER51114 and W-7405-ENG-48 *Lawrence Livermore National Laboratory GENERAL ATOMICS PROJECT 3466 FEBRUARY 1995 ASTER DISTRIBUTION QE IHIS DACUlvlENT IS UNIJ^O Ul ' ' *|* GENERAL ATOMICS DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof. -
Anl-7807 Anl-7807 Survey of Thermonuclear-Reactor
ANL-7807 ANL-7807 SURVEY OF THERMONUCLEAR-REACTOR PARAMETERS P. J. Persiani, W. C. Lipinski, and A. J. Hatcli U of C-AUA-USAECB ARGONNE NATIONAL LABORATORY, ARGONNE, ILLINOIS Prepared for the U.S. ATOMIC ENERGY COMMISSION under Contract W-31-109-Eng-38 The faciliUes of Argonne National Laboratory are owned by the "-'f •> S'^^f °°^^%'" ment. Under the terms of a contract (W-31-109-Eng-38) between the U. S. ""^^^^J^^'J/ Commission, Argonne Universities Association and The University of Chicago, the ""'J'"=">' employs the staff and operates the Laboratory in accordance with policies and programs formu- lated, approved and reviewed by the Association. MEMBERS OF ARGONNE UNIVERSITIES ASSOCIATION The Ohio State University The University of Arizona Kansas State University Carnegie-Mellon University The University of Kansas Ohio University Case Western Reserve University Loyola University The Pennsylvania State University The University of Chicago Marquette University Purdue University University o£ Cincinnati Michigan State University Saint Louis University Illinois Institute of Technology The University of Michigan Southern Illinois University University of Illinois University of Minnesota The University of Texas at Austin Indiana University University of Missouri Washington University Iowa State University Northwestern University Wayne State University The University of Iowa University of Notre Dame The University of Wisconsin NOTICE This report was prepared as an account of work sponsored by the United States Government. Neither the United States nor the United States Atomic Energy Commission, nor any of their employees, nor any of their contractors, subcontrac tors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness or usefulness of any information, apparatus, product or process disclosed, or represents that its use would not infringe privately-owned rights. -
Physics and Computational Simulations of Plasma Burn-Through for Tokamak Start-Up
Imperial College London Department of Physics Physics and Computational Simulations of Plasma Burn-through for Tokamak Start-up Hyun-Tae Kim Submitted in part fulfilment of the requirements for the degree of Doctor of Philosophy in Physics of Imperial College London, July 2013 Abstract This thesis will discuss the fundamental process of high temperature plasma formation, con- sisting of the Townsend avalanche phase and the subsequent plasma burn-through phase. By means of the applied electric field, the gas is partially ionized by the avalanche process. In order for the electron temperature to increase, the remaining neutrals need to be fully ionized in the plasma burn-through phase, as radiation is the main contribution to the electron power loss. The radiated power loss can be significantly affected by impurities resulting from inter- action with the plasma facing components. The parallel transport to the surrounding walls is determined by the so called connection length in the plasma. Previously, plasma burn-through was simulated with the assumptions of constant particle con- finement time and impurity fraction. In the new plasma burn-through simulator, called the DYON code, the treatment of particle confinement time is improved with a transonic ambipo- lar model for parallel transport, by using the effective connection length determined by the magnetic field lines, and Bohm diffusion model for perpendicular transport. In addition, the dynamic evolution of impurity content is calculated in a self-consistent way, using plasma wall interaction models. The recycling of the particles at the walls is also modelled. For a specific application, the recent installation of a beryllium wall at Joint European Torus (JET) enabled to investigate the effects of plasma facing components on plasma formation and build-up of plasma current in the device. -
Effect of Quaslconflned Particles and I= 2 Stellarator Fields on the Negative Mass Lnstablllty in a Modified Betatron G
TABLE II. Coefficients a and b + r of log(ac,) vs log[2/( p 1/p0 +Pel ACKNOWLEDGMENTS p,)J. We thank Jeanette Nelson for a careful reading of the log(ac1 ) =a+ b log(2/( pc/p1 + p 1/p0 ) l when a = 10 manuscript and G. Pollarolo for useful discussions about the NAG FORTRAN LIBRARY. The numerical computations were 0.1 <Pi <Po< 10 carried out on the Vax 11/780 ofINFN Sezione di Torino. M = 100 M=30 M =IO a; b; r 0.44; 0.06; 0.99 0.33; 0.06; 0.98 0.42; 0.04; 0.98 1 where r0 is the Lorentz factor and spans between 1 and 10. A. E. Gill, Phys. Fluids 8, 1428 (1965). The presence of a shear in cylindrical symmetry has not 2 A. Ferrari, B. Trusooni, and L. Zaninetti, Mon. Not. R. Astron. Soc. 196, yet been considered and will presumably produce a cutoff in !OSI (1981). 3H. Cohn, Astrophys. J. 269, 500 (1983). the instabilities where a> 21'Id, with d (in jet radius units) 4 D. G. Payne and H. Cohn, Astrophys. J. 287, 29S (1984). the length characterizing the thickness of the shear. ' A. M. Anile, J.C. Miller, and S. Motta, Phys. Fluids 26, 14SO (1983). Effect of quaslconflned particles and I= 2 stellarator fields on the negative mass lnstablllty in a modified betatron G. Roberts and N. Rostoker Department ofPhy sics, University ofCalifomia, Irvine. California 92717 (Received 5 February 1985; accepted 10 October 1985) A sufficient stability condition for the negative mass instability is derived. -
50 Years of Fusion Research
IOP PUBLISHING and INTERNATIONAL ATOMIC ENERGY AGENCY NUCLEAR FUSION Nucl. Fusion 50 (2010) 014004 (14pp) doi:10.1088/0029-5515/50/1/014004 50 years of fusion research Dale Meade Fusion Innovation Research and Energy®, 48 Oakland Street, Princeton, NJ 08540, USA E-mail: [email protected] Received 6 August 2009, accepted for publication 16 November 2009 Published 30 December 2009 Online at stacks.iop.org/NF/50/014004 Abstract Fusion energy research began in the early 1950s as scientists worked to harness the awesome power of the atom for peaceful purposes. There was early optimism for a quick solution for fusion energy as there had been for fission. However, this was soon tempered by reality as the difficulty of producing and confining fusion fuel at temperatures of 100 million ◦C in the laboratory was appreciated. Fusion research has followed two main paths— inertial confinement fusion and magnetic confinement fusion. Over the past 50 years, there has been remarkable progress with both approaches, and now each has a solid technical foundation that has led to the construction of major facilities that are aimed at demonstrating fusion energy producing plasmas. PACS numbers: 52.55.−s, 52.57.−z, 28.52.−s, 89.30.Jj (Some figures in this article are in colour only in the electronic version) 1. Introduction—fusion energy prior to 1958 2. Two main approaches to fusion energy The 1950s were a period of rapid progress and high It was understood very early on that fusion fuel temperatures of several hundred million ◦C would be needed to initiate expectations in science and technology. -
Publ. Astron. Obs. Belgrade No. 99 (2020), 256 - 257 Invited Lecture
Publ. Astron. Obs. Belgrade No. 99 (2020), 256 - 257 Invited Lecture CHALLENGES AND PROGRESS ON THE PATH TOWARDS FUSION ELECTRICITY A. J. H. DONNÉ EUROfusion, Garching, Germany E-mail [email protected] Abstract. The European Roadmap to the Realisation of Fusion Energy1 breaks the quest for fusion energy into eight missions: 1. Plasma regimes of operation: Demonstrate plasma scenarios (based on the tokamak configuration) that increase the success margin of ITER and satisfy the requirements of DEMO. 2. Heat-exhaust systems: Demonstrate an integrated approach that can handle the large power leaving ITER and DEMO plasmas. 3. Neutron tolerant materials: Develop materials that withstand the large 14MeV neutron flux for long periods while retaining adequate physical properties. 4. Tritium self-sufficiency: Find an effective technological solution for the breeding blanket that also drives the generators. 5. Implementation of the intrinsic safety features of fusion: Ensure safety is integral to the design of DEMO using the experience gained with ITER. 6. Integrated DEMO design and system development: Bring together the plasma and all the systems coherently, resolving issues by targeted R&D activities 7. Competitive cost of electricity: Ensure the economic potential of fusion by minimising the DEMO capital and lifetime costs and developing long-term technologies to further reduce power plant costs. 8. Stellarator: Bring the stellarator line to maturity to determine the feasibility of a stellarator power plant. Now we are approaching the end of the 8th European Framework Programme (2014- 2020), it is a good moment to look back at the achievements since the establishment of EUROfusion in 2014, while at the same time have a peek into the future, to see which challenges lay ahead of us as well as the strategy to tackle them. -
Observation of Nuclear Fusion Driven by a Pyroelectric Crystal
letters to nature 1900þ14. I. An interpretive study of BeppoSAX and Ulysses observations. Astrophys. J. 549, electrostatic field of the crystal is used to generate and accelerate 1021–1038 (2001). a deuteron beam (>100 keV and >4 nA), which, upon striking a 10. Gaensler, B. M. et al. Second-epoch VLA observations of SGR 1806220. GRB Circ. Network 2933 (2005). deuterated target, produces a neutron flux over 400 times the 11. Corbel, S. & Eikenberry, S. S. The connection between W31, SGR 1806220, and LBV 1806220: background level. The presence of neutrons from the reaction Distance, extinction, and structure. Astron. Astrophys. 419, 191–201 (2004). D 1 D ! 3He (820 keV) 1 n (2.45 MeV) within the target is 12. Kolpak, M. A., Jackson, J. M., Bania, T. M. & Dickey, J. M. The radial distribution of cold atomic hydrogen in the galaxy. Astrophys. J. 578, 868–876 (2002). confirmed by pulse shape analysis and proton recoil spectro- 13. Corbel, S. et al. The distance of the soft gamma repeater SGR 1806220. Astrophys. J. 478, 624–630 scopy. As further evidence for this fusion reaction, we use a novel (1997). time-of-flight technique to demonstrate the delayed coincidence 14. Hartmann, D. & Burton, W. B. Atlas of Galactic Neutral Hydrogen. Ch. 4, 169 (Cambridge Univ. Press, between the outgoing a-particle and the neutron. Although the Cambridge, 1997). 15. Garwood, R. W. & Dickey, J. M. Cold atomic gas in the inner Galaxy. Astrophys. J. 338, 841–861 (1989). reported fusion is not useful in the power-producing sense, we 16. Figer, D. -
Astron 104 Laboratory #7 Nuclear Fusion and Stars Chapter 12
Lab #7 Name: Date: Section: Astron 104 Laboratory #7 Nuclear Fusion and Stars Chapter 12 Introduction You are intimately linked to the nuclear fusion that occurs in stars. Life on Earth thrives on sunlight, which originates as energy produced at the center of the Sun as hydrogen is fused to form helium. Even the very atoms and molecules of your body | iron in your blood, calcium in your bones, phosphorous in your DNA | were forged in stars and dispersed to the interstellar medium in spectacular explosions. In this lab, you will explore the creation of heavy elements and release of energy through nuclear fusion in stars. Learning Objectives At the completion of this lab, you should be able to: 1. Describe the components of atomic nuclei and the properties of subatomic particles 2. Describe the force between two protons as a function of their separation distance 3. Describe the temperature required for nuclear fusion of hydrogen and heavier elements 4. Describe how nuclear fusion produces energy 5. Describe why iron is the heaviest element that can be made via nuclear fusion in stars Atomic Nuclei [5 pts each, 15 pts total] Atomic nuclear are made of combinations of sub-microscopic particles called protons and neutrons. The neutron is slight more massive than the proton, but for now we will ignore that difference and assume the neutron and proton each have a mass of 1 unit. Protons have a positive electrical charge (let's call it +1 unit) and neutrons have no electrical charge. Astron 104 Fall 2015 1 Lab #7 1.