Fusion Cross-Sections for Deuterium Cycle Reactors

Total Page:16

File Type:pdf, Size:1020Kb

Fusion Cross-Sections for Deuterium Cycle Reactors Fusion cross-sections for deuterium cycle fusion reactors (D-cycle): an analysis of geometric, Gamow- Sommerfeld and astrophysical S-factors Abstract Fusion reactions in the deuterium cycle (D+D, D+T and D+3He) are the main nucleus-nucleus interactions which occur in tokamaks and stellerators. These reactions are the limiting case between the Woods-Saxon potential field at nuclear distances and the Coulomb electrostatic potential (scattering) at longer distances. In this paper several fusion cross-sections, geometric, Gamow- Sommerfeld and astrophysical S-factors have been reviewed and compared with experimental data from the last ENDF/B-VIII.0 cross-section library. The XDC-fusion code has been developed to calculate fusion cross-sections, geometric, Gamow-Sommerfeld and S-factors of the deuterium-cycle (D-cycle), including resonance parameters (energy and partial width). The software estimates also fusion reaction heat (Q) and Woods-Saxon/Coulomb proximity potentials. Although relative differences between fusion cross-sections are lower than 5 %, S-factors present considerable differences between the energies and partial width (FWHM) of the single-level Breit-Wigner (SLBW) resonances. The energy at which is placed the maximum fusion cross-section is also different between cases. In conclusion, fusion reaction models for light nuclei (deuterium, tritium and helium) should be reviewed in order to apply fusion to energy production in safety conditions. Keywords: Fusion reaction, fusion cross-section, astrophysical S-factor, Gamow-Sommerfeld factor 1. Introduction Fusion reactions in the deuterium cycle (D+D, D+T and D+3He) are the main nucleus-nucleus interactions which occur in the deuterium cycle (D-cycle) in tokamaks and stellerators fusion reactors [Smith and Cowley 2010, Donné 2018, Zohm 2019]. Fusion reactions are the limiting case between the Woods-Saxon potential field at nuclear distances and the Coulomb electrostatic potential (scattering) at longer distances. In order to overpass the Coulomb electrostatic barrier and achieve nuclear distances to allow fusion reactions, ionized plasma is confined by a magnetic field inside tokamaks and stellerators [Knoepfel 1978, Woods 2006] Fusion reactions are characterized by their fusion cross-sections and described by three energy dependent functions: geometric, Gamow-Sommerfeld and astrophysical S-factor. These factors retain the physical characteristics of fusion reaction: a Coulomb electrostatic potential barrier penetration, in a form of an exponential attenuation, G(E), and a strong force interaction after tunneling effect in the nuclear potential well (Woods-Saxon), at the boundary conditions, in a form of an astrophysical S(E) factor or resonance function [Miley et al 1974, Li 2002, Chen 2016]. Fusion cross section is expressed in a simplified form as f (E) GS where ϕ is the geometric factor, a term inversely proportional with incident particle energy, S is a strong-energy correlated parameter S-factor, called also astrophysical or S-factor, which depends on the boundary conditions between nuclear well and Coulomb electrostatic field and G(E), a tunneling or penetration factor, called Gamow-Sommerfeld factor. In particular, the astrophysical S-factor is a resonance function, based on the classical formula of Breit-Wigner of single-level resonances [Breit and Wigner 1936]. Fusion cross-section of light nuclei were firstly estimated by the Naval Research Laboratory, who published a 5 parameter formula for D+D, D+T and D+3He light nuclei fusion reactions, also known as Duane 5-parameter formula, based on accelerator beam-target experiments [NRL 2019]. Corresponding author: [email protected] Further studies, such as those carried out by Bosch and Hale in 1992, included a 9 parameter formula for Gamow and S-factor, based on the R-matrix of thousand experiments, and an inverse energy dependent geometric factor. However, in the case of D(d,p)T fusion reaction, no resonance peak was included [Bosch and Hale 1992]. In the last decades, fusion cross-sections have been modeled with a complex phase-shift of the incident wavefunction at the boundaries of Coulomb electrostatic potential and Woods-Saxon potential for the nuclear well, including SLBW resonance peaks for all target nuclei (D, T or 3He) [Li et al 2006,2008, Singh et al 2019]. In order to estimate fusion cross-section, geometric, Gamow-Sommerfeld, S-factors and SLBW resonance parameters in the D-cycle, the XDC-fusion code has been developed. Fusion cross-sections equations estimated through different expression have been compared with ENDF/B-VIII.0 cross- section libraries: Duane 5-parameter formula, Bosch-Hale 9-parameter formula and a combined geometric factor based on wavenumber and a complex phase-shift S-factor. 2. The D-cycle The deuterium cycle of fusion is composed of several interdependent nuclear reactions [Atzeni and Meyer-ter-Vehn 2001, Ball 2019]: 2 2 3 1 1 D + 1 D 1T (1.01 MeV) + 1 H ( 3.02 MeV) 2 2 3 1 1 D + 1 D 2 He (0.82 MeV) + 0 n ( 2.45 MeV) 2 3 4 1 1 D + 1T 2 He (3.52 MeV) + 0 n (14.07 MeV) 2 3 4 1 1 D + 2 He 2 He (3.67 MeV) + 1 H (14.68 MeV) which can be summarized in 2 4 1 1 6 1 D 2 He (3.52 MeV) + 1 H (3.02 MeV) + 0 n (14.07 MeV) 4 1 1 2 He (3.67 MeV) + 1 H (14.68 MeV) + 0 n (2.45 MeV) + 1.83 MeV Furthermore, protons produced by fusion reactions can also react with low probability as 1 1 2 1 H + 1 H 1 D + e + + 0.93 MeV (99.76 %) 1 1 2 1 H + 1 H + e 1 D + + 1.95 MeV (0.24 %) Other fusion reactions of the deuterium cycle with a low branching ratio are [Robouch et al 1993, Bystritsky et al 1998] 2 2 4 1 D + 1 D 2 He (0.08 MeV) + γ0(23.77 MeV) and with tritium as target nuclei 2 3 4 1 1 D + 1T 2 He (3.52 MeV) + 0 n (14.07 MeV) 2 3 5 * 1 D + 1T 2 He (0.05 MeV) + γ0(16.65 MeV) 2 3 5 * 1 D + 1T 2 He (3.2 MeV) + γ1(13.50 MeV) There are other fusion reactions in which the reaction heat is positive, which have not been considered, such as 2 3 3 1 1 D + 1T 2 He + 2 0 n 2 3 3 1 1 1 D + 2 He 2 He + 1 H + 0 n Table 1 summarizes the main characteristics of the D-cycle fusion: branching ratios (BR), reaction heat (Q) and emergent particle/gamma energies. 3. Geometric, Gamow-Sommerfeld and S-factor 3.1. Geometric factor (ϕ) In most of the fusion cross-section expressions, geometric factor is expressed as 1/ E . In the last decades, geometric factor has been expressed as the area subtended by a de Broglie wavelength or wavenumber k, which depends on energy [Li et al 2006, 2008] (E) 2 k 2 with k 2E / where μ is the reduced mass of the system, m1m2 / m1 m2 The geometric factor ϕ(E) can also be expressed with two independent terms, 2 1 (E) 2 E The first term is a conversion factor which is included in some expressions in the Gamow-Sommerfeld or in the S-factor, with units of keV.b in the SI. 3.2. Gamow-Sommerfeld factor 3.2.1 Introduction The Gamow-Sommerfeld factor G(E) is a penetration factor of the Coulomb barrier by the incident particle and characterize the probability of incident/target nuclei of reaching a fusion reaction. It is expressed with an exponential attenuation function as [Brennan and Coyne 1964, Humblet et al 1987] 1 G(E) exp 2 2 l with ηl the Sommerfeld parameter, evaluated as r 1 tp k (r) dr l l rn with kl the wave number inside the nuclear well 1/ 2 2 k (r) E U(r) l 2 where U(r) is the potential field, rn is the classical distance of closest approach (nuclear square-well radius) and rtp is the classical turning point, that is, the distance in which the energy of the incident particle energy is E U (rtp ) [Lee and Jung 2017] 3.2.2 Case 1: Duane parametrization Duane parametrization included an interpolation of the Gamow factor as the Mott’s form of the Coulomb barrier penetrability [Mott and Massey 1965, NRL 2019] 1 G(E) exp A1/ E 1 3.2.3 Case 2 Let us consider that the potential field U(r) can be approximated as 2ll 1 U (r) U (r) C 2 r 2 where UC is the Coulomb potential and the second term is the spin-orbit potential, with l the magnetic quantum number. The Coulomb electrostatic potential is expressed as Z Z e2 U (r) k 1 2 r r C e r n with ke 1/ 4 0 the Coulomb electrostatic constant and rn is estimated as 1/3 1/3 rn r0 A1 A2 with r0 the specific radius per nucleon of fusion reaction and the classical turning point rtp as 2 rtp keZ1Z2e / E The centrifugal term is zero at the boundaries of the nuclear potential well (l=0), then the integral is calculated as [Atzeni 2004] 1 B E E E g arccos 1 0 2 E U U U 0 0 0 where rtp U0 U (rn ) E rn and 1/ 2 2 2 Bg g 2 keZ1Z2e / 2 is the Gamow constant. The η0 can be also expressed in term of the lengths rn and rtp as 1 B r r r g n n n 0 arccos 1 2 E r r r tp tp tp 1/ 2 The arccosine can be expanded in powers of E /U 0 , thus 1/ 2 3/ 2 5/ 2 1 Bg E 1 E 3 E E E ..
Recommended publications
  • Varying Constants, Gravitation and Cosmology
    Varying constants, Gravitation and Cosmology Jean-Philippe Uzan Institut d’Astrophysique de Paris, UMR-7095 du CNRS, Universit´ePierre et Marie Curie, 98 bis bd Arago, 75014 Paris (France) and Department of Mathematics and Applied Mathematics, Cape Town University, Rondebosch 7701 (South Africa) and National Institute for Theoretical Physics (NITheP), Stellenbosch 7600 (South Africa). email: [email protected] http//www2.iap.fr/users/uzan/ September 29, 2010 Abstract Fundamental constants are a cornerstone of our physical laws. Any constant varying in space and/or time would reflect the existence of an almost massless field that couples to mat- ter. This will induce a violation of the universality of free fall. It is thus of utmost importance for our understanding of gravity and of the domain of validity of general relativity to test for their constancy. We thus detail the relations between the constants, the tests of the local posi- tion invariance and of the universality of free fall. We then review the main experimental and observational constraints that have been obtained from atomic clocks, the Oklo phenomenon, Solar system observations, meteorites dating, quasar absorption spectra, stellar physics, pul- sar timing, the cosmic microwave background and big bang nucleosynthesis. At each step we arXiv:1009.5514v1 [astro-ph.CO] 28 Sep 2010 describe the basics of each system, its dependence with respect to the constants, the known systematic effects and the most recent constraints that have been obtained. We then describe the main theoretical frameworks in which the low-energy constants may actually be varying and we focus on the unification mechanisms and the relations between the variation of differ- ent constants.
    [Show full text]
  • The Α-Decay in Ions and Highly Compressed Matter
    Alpha decay in electron environments of increasing density: from the bare nucleus to compressed matter Fabio Belloni* European Commission, Joint Research Centre, Institute for Transuranium Elements Postfach 2340, D-76125 Karlsruhe, Germany E-mail: [email protected] Abstract The influence of the electron environment on the α decay is elucidated. Within the frame of a simple model based on the generalized Thomas-Fermi theory of the atom, it is shown that the increase of the electron density around the parent nucleus drives a mechanism which shortens the lifetime. Numerical results are provided for 144Nd, 154Yb and 210Po. Depending on the nuclide, fractional lifetime reduction relative to the bare nucleus is of the order of 0.1÷1% in free ions, neutral atoms and ordinary matter, but may reach up to 10% at matter densities as high as 104 g/cm3, in a high-Z matrix. The effect induced by means of state-of-the-art compression techniques, although much smaller than previously found, would however be measurable. The extent of the effect in ultra-high-density stellar environments might become significant and would deserve further investigation. * Presently at: European Commission, Directorate-General for Research & Innovation, Directorate Energy, Rue du Champ de Mars 21, 1049 Brussels, Belgium. 1 1. Introduction Whether and to which extent the α-decay width might be modified in electron environments has been the subject of numerous theoretical and experimental investigations, boomed over the last years. It has indeed been put forward that this effect could have implications in the stellar nucleosynthesis of heavy elements [1,2], with an impact on nuclear cosmochronology [3] (e.g.
    [Show full text]
  • Nuclear Fusion Reactions of Interest to Controlled Energy Production Had Been Established
    Nuclear fusion 1 reactions 1.1 Exothermic nuclear Most of this book is devoted to the physical principles of energy produc- reactions: fission and tion by fusion reactions in an inertially confined medium. To begin with, fusion 2 in this chapter we briefly discuss fusion reactions. 1.2 Fusion reaction physics 3 We first define fusion cross section and reactivity, and then present and 1.3 Some important fusion justify qualitatively the standard parametrization of these two important reactions 10 quantities. Next, we consider a few important fusion reactions, and pro- 1.4 Maxwell-averaged vide expressions, data, and graphs for the evaluation of their cross sections fusion reactivities 14 and reactivities. These results will be used in the following chapters to 1.5 Fusion reactivity in very derive the basic requirements for fusion energy production, as well as to high density matter 21 study fusion ignition and burn in suitable inertially confined fuels. 1.6 Spin polarization of In the last part of this chapter, we also briefly discuss how high material reacting nuclei 24 density and spin polarization affect fusion reactivities. Finally, we outline 1.7 µ-catalysed fusion 25 the principles of muon-catalysed fusion. 1.8 Historical note 27 Atzeni: “chap01” — 2004/4/29 — page1—#1 2 1.1 Exothermic nuclear reactions: fission and fusion 1.1 Exothermic nuclear reactions: fission and fusion According to Einstein’s mass–energy relationship, a nuclear reaction in which the total mass of the final products is smaller than that of the reacting nuclei is exothermic, that is, releases an energy Reaction Q 2 Q = mi − mf c 1.1 i f proportional to such a mass difference.
    [Show full text]
  • Stellar Nucleosynthesis
    Stellar nucleosynthesis Stellar nucleosynthesis is the creation (nucleosynthesis) of chemical elements by nuclear fusion reactions within stars. Stellar nucleosynthesis has occurred since the original creation of hydrogen, helium and lithium during the Big Bang. As a predictive theory, it yields accurate estimates of the observed abundances of the elements. It explains why the observed abundances of elements change over time and why some elements and their isotopes are much more abundant than others. The theory was initially proposed by Fred Hoyle in 1946,[1] who later refined it in 1954.[2] Further advances were made, especially to nucleosynthesis by neutron capture of the elements heavier than iron, by Margaret Burbidge, Geoffrey Burbidge, William Alfred Fowler and Hoyle in their famous 1957 B2FH paper,[3] which became one of the most heavily cited papers in astrophysics history. Stars evolve because of changes in their composition (the abundance of their constituent elements) over their lifespans, first by burning hydrogen (main sequence star), then helium (red giant star), and progressively burning higher elements. However, this does not by itself significantly alter the abundances of elements in the universe as the elements are contained within the star. Later in its life, a low-mass star will slowly eject its atmosphere via stellar wind, forming a planetary nebula, while a higher–mass star will eject mass via a sudden catastrophic event called a supernova. The term supernova nucleosynthesis is used to describe the creation of elements during the explosion of a massive star or white dwarf. The advanced sequence of burning fuels is driven by gravitational collapse and its associated heating, resulting in the subsequent burning of carbon, oxygen and silicon.
    [Show full text]
  • PHY401: Nuclear and Particle Physics
    PHY401: Nuclear and Particle Physics Lecture 19, Monday, October 5, 2020 Dr. Anosh Joseph IISER Mohali Nuclear Fusion PHY401: Nuclear and Particle Physics Dr. Anosh Joseph, IISER Mohali Nuclear Fusion Let us look at the plot of average binding energy per nucleon against mass number. It has a maximum at A ≈ 56. And after that it slowly decreases for heavier nuclei. The decrease is much quicker for lighter nuclei. PHY401: Nuclear and Particle Physics Dr. Anosh Joseph, IISER Mohali Nuclear Fusion PHY401: Nuclear and Particle Physics Dr. Anosh Joseph, IISER Mohali Nuclear Fusion Lighter nuclei are less tightly bound than medium-size nuclei (exception: magic nuclei). Thus, in principle, energy could be produced by two light nuclei fusing to produce a heavier, and more tightly bound nucleus. This is process of inverse to fission. PHY401: Nuclear and Particle Physics Dr. Anosh Joseph, IISER Mohali Nuclear Fusion Just as for fission, the energy released comes from difference in the binding energies of initial and final states. This process is called nuclear fusion. Very attractive as a potential source of power... ... because of the far greater abundance of stable light nuclei in nature than very heavy nuclei. PHY401: Nuclear and Particle Physics Dr. Anosh Joseph, IISER Mohali Nuclear Fusion Thus fusion would offer enormous potential for power generation, if ... ...the huge practical problems could be overcome. Fusion processes also explain how stars are formed. PHY401: Nuclear and Particle Physics Dr. Anosh Joseph, IISER Mohali Coulomb Barrier Practical problem to obtaining fusion has its origin in Coulomb repulsion. It inhibits two nuclei getting close enough together to fuse.
    [Show full text]
  • Chapter 4 Nuclear Reactions: BBN, Stars, Etc This Chapter Is Divided
    Chapter 4 Nuclear Reactions: BBN, Stars, etc This chapter is divided into three parts: • preliminaries: thermally averaged rates and the S-factor • application to the pp chain • He burning 4.1 Rates and cross sections We want to consider the reaction 0 0 1(p1) + 2(p2) ! 1 (p10 ) + 2 (p20 ) where the four-momentum of particle 1 is given by p1, etc. The rate (events/unit time in some volume V) is Z Z 3 3 dN m1m2 2 4 4 m10 d p10 m20 d p20 0 0 = d~xρ1(p1; ~x) ρ2(p2; ~x) jMfij (2π) δ (p1 + p2 − p1 − p2) 3 3 dt E1E2 (2π) E10 (2π) E20 Z m1m2 = d~xρ1(p1; ~x) ρ2(p2; ~x) j~v1 − ~v2j σ12(p1; p2) (1) E1E2 where ρ1(p1; ~x) is the number density of particles of type 1 with four-momentum p1 (that is, the number of particles per unit volume). The relative velocity is defined p 2 2 2 (p1 · p2) − m1m2 j~v1 − ~v2j = (2) E1E2 Suppose the densities above are constant over the volume of interest (some region within a star). Then the integral over ~x is simple, yielding 1 dN ρ1ρ2 r = events=unit time=unit volume = = j~v1 − ~v2jσ12 (3) V dt 1 + δ12 Note the factor of 1 + δ12. The rate should be proportional to the number of pairs of P interacting particles in the volume. If the particles are distinct, this is ij / ρ1ρ2, but if 1 P 1 the particles are identical, the sum over distinct pairs gives 2 ij / 2 ρ1ρ2.
    [Show full text]
  • Measuring the Neon-20 Radiative Proton Capture Rate at Dragon
    MEASURING THE NEON-20 RADIATIVE PROTON CAPTURE RATE AT DRAGON by Jonathan Karpesky c Copyright by Jonathan Karpesky, 2020 All Rights Reserved A thesis submitted to the Faculty and the Board of Trustees of the Colorado School of Mines in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Physics). Golden, Colorado Date Signed: Jonathan Karpesky Signed: Dr. Uwe Greife Thesis Advisor Golden, Colorado Date Signed: Dr. Uwe Greife Professor and Head Department of Physics ii ABSTRACT Understanding the abundance levels of isotopes produced in oxygen-neon (ONe) novae within our galaxy requires accurate measurements of nuclear reaction rates within their associated reaction networks. During these cataclysmic events, the produced radioisotope 22Na is ejected into the interstellar medium and β-decays predominately to the first excited state in 22Ne leading to a characteristic 1.275 MeV γ-ray. To date, there has been no astronomical observation of this characteristic γ-ray that can be a potential probe into the physics occuring within novae. The production of 22Na in classical novae is limited by the 20Ne(p,γ)21Na nuclear reaction that is the focus of this experiment. Using the DRAGON recoil separator, new measurements of the 20Ne(p,γ)21Na reaction are performed at center-of- mass energies ranging from 265.5 - 519.6 keV that reach towards the astrophysically relevant energy ranges. The goal is to reduce experimental uncertainties in the 20Ne(p,γ)21Na reaction rate in order to be able to constrain the astrophysical S-factor. In addition, in the frame of this thesis a differential cross-section measurement was performed of 3He + p scattering to test the performance of the new Colorado School of Mines designed and built SONIK scattering chamber.
    [Show full text]
  • Republic of Iraq Ministry of Higher Education and Scientific Research University of Baghdad College of Education for Pure Sciences( Ibn Al-Haitham)
    Republic of Iraq Ministry of Higher Education And Scientific Research University of Baghdad College of Education for pure Sciences( Ibn Al-Haitham) Quantum Mechanics Consideration For Fusion Cross Section A Thesis Submitted to the Council of College of Education for pure Sciences (Ibn Al-Haitham) University of Baghdad in Partial Fulfillment of the Requirements for the Degree of Master in Nuclear Physics By Muayad Mohammed Abed Supervisor Assist. Prof .Dr.Raad Hameed Majeed Assist Prof. Dr. Mustafa Kamel Jassim 2014 A.D 1435 H.D Acknowledgments In the beginning, praise is to Allah for helping me in everything. I would like to express my deepest gratitude to everyone who has given me the support I needed to complete this thesis .My deep appreciation goes to to Assist Prof. Dr. Raad Hameed Majeed for supervision and thanks to Assist Prof. Dr. Mustafa Kamel Jassim for his help, continuous help and useful discussion during the preparation of this work and Assist Prof. Dr. Hadi Alagealy for his help. Finally , I would like to thank my dearest people (my parents , brothers , my wife and my children ) have been the greatest role in supporting me to accomplish this work with their continuous encouragement and prayers . Muayad Supervisor's Certification We certify that this thesis was prepared under our supervision at University of Baghdad / College of Education Ibn- Al – Haitham / Department of Physics in partial fulfillment of the requirements for the degree of Master of Science in Physics. Signature: Signature: Supervisor: Dr.Raad H .Majeed Supervisor: Dr.Mustafa K. Jassim Title: Assist Professor Title: Assist Professor Department of physics Department of Physics College of Ibn-Al- Haitham College of Ibn-Al-Haitham University of Baghdad University of Baghdad Date: / / 2014 Date: / /2014 In view of the available recommendation, we forward this thesis for debate by the examining committee.
    [Show full text]
  • The Gamow Peak and the Reaction Rate • Reaction Rates and Temperature
    Nuclear reactions of astrophysical interest • Introduction • Scales of energy and density • Reaction rate • Neutron induced processes • Cross sections of charged particles • Astrophysical factors • The Gamow peak and the reaction rate • Reaction rates and temperature 1 Introduction • Most important processes are neutron induced reactions: n + AZ →A+1Z + g • and reactions between nuclei A1 A2 → A Z1+ Z2 Z+X • The first reactions are relevant when one has free neutrons, as in the big bang and /or in advanced stellar phases where neutrons are produced , (e.g.. 22Ne+4He → 25Mg +n ) or from neutronization reactions • Reaction between nuclei are important for forming heavier elements,as in the big bang and/or in stellar combustion 2 ro Scales of energy and angular momentum p • The collision energies of interest to us are generally smaller than the typical nuclear energy scale, order 1MeV: • Indeed, primordial nucleosysnthesis becomes effective at kT<100 keV, otherwise the first products (deuterons) disintegrate through photodissociation • Nucleosynthesis in the Sun occurs at kT ≈ 1keV; Helium burning stars have KT ≈10KeV • Typical momenta are thus p ≈ (kT m)1/2 ; Put mc2=1GeV e kT=100 KeV . One gets p ≈ 10 MeV/c • Since the typical nuclear dimensions are r0 ≈ 1fm the angular momentum involved for the nuclear collision is, classically, L=p r0 = 10(MeV/c fm) ≈ (1/20) ħ, thus the dominant processes are dominated by the smallest angular momenta, compatible with quantum mechanics. 3 Note I: cross section • The cross section is the main statistical quantity which characterizes a collision process. • Suppose you study A+B→C+D by shooting a beam of particle A onto a target of B • The beam is characterized by the “current ” I (number of particles produced per unit time), by the particle type and energy.
    [Show full text]