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R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 1 Nuclear Forces - Lecture 1 - R. Machleidt University of Idaho History, Facts and.

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Presentation on theme: "R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 1 Nuclear Forces - Lecture 1 - R. Machleidt University of Idaho History, Facts and."— Presentation transcript:

1 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 1 Nuclear Forces - Lecture 1 - R. Machleidt University of Idaho History, Facts and Phenomenology 12th CNS International Summer School (CNSSS13) 28 August to 03 September 2013 -- CNS Wako Campus

2 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 2 Nuclear Forces - Overview of all lectures - Lecture 1: History, facts, and phenomenology Lecture 2: The meson theory of nuclear forces Lecture 3: QCD and nuclear forces; effective field theory (EFT) for low-energy QCD Lecture 4: Nuclear forces from chiral EFT

3 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 3 Lecture 1: History, Facts, and Phenomenology  Historical review  Properties of the nuclear force  Phenomenological descriptions

4 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 4 History of Nuclear Forces: Phase I 1930’s Chadwick (1932): Neutron Heisenberg (1932): First Phenomenology (Isospin)

5 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 5 Heisenberg and his contribution of 1932 Heisenberg Niels Bohr Pauli

6 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 6 Zeitschrift fuer Physik 77, 1 (1932) On the Structure of Atomic Nuclei. I. …. … Chadwick … … suggests the assumption that atomic nuclei are built from protons and neutrons without electrons …

7 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 7 Zeitschrift fuer Physik 77, 1 (1932), cont’d Precursor of the idea of Boson Exchange! … the force … between proton and neutron … ….. in analogy to the H2+-ion --- an exchange of negative charge will take place, … This exchange can be visualized by electrons which do not have spin and follow the rules of bose statistics …

8 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 8 History, Phase I cont’d 1930’s Chadwick (1932): Neutron Heisenberg (1932): First Phenomenology (Isospin) Yukawa (1935): Meson Hypothesis

9 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 9 Yukawa and his idea S. Tomonaga, H. Yukawa, and S. Sakata in the 1950s. Tomonaga Yukawa Sakata

10 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 10 From: H. Yukawa, Proc. Phys. Math. Soc. Japan 17, 48 (1935).

11 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 11

12 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 12

13 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 13 History, Phase I cont’d 1930’s Chadwick (1932): Neutron Heisenberg (1932): First Phenomenology (Isospin) Yukawa (1935): Meson Hypothesis 1950’s Taketani, Nakamura, Sasaki (1951): 3 ranges. One-Pion-Exchange (OPE): o.k. Multi-pion exchanges: Problems! Taketani, Machida, Onuma (1952); Brueckner, Watson (1953). Quotes by Bethe (1953) and Goldberger (1960) “Pion Theories” Discovery of the pion in cosmic ray (1947) and in the Berkeley Cyclotron Lab (1948). Nobelprize awarded to Yukawa (1949). 1940’s

14 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 14 Scientific American, September 1953 What Holds the Nucleus Together? by Hans A. Bethe In the past quarter century physicists have devoted a huge amount of experimentation and mental labor to this problem – probably more man-hours than have been given to any other scientific question in the history of mankind.

15 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 15 “There are few problems in nuclear theoretical physics which have attracted more attention than that of trying to determine the fundamental interaction between two nucleons. It is also true that scarcely ever has the world of physics owed so little to so many … … It is hard to believe that many of the authors are talking about the same problem or, in fact, that they know what the problem is.” M. L. Goldberger Midwestern Conference on Theoretical Physics, Purdue University, 1960

16 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 16 History, Phase I (The first pion period) 1930’s Chadwick (1932): Neutron Heisenberg (1932): First Phenomenology (Isospin) Yukawa (1935): Meson Hypothesis 1950’s Taketani, Nakamura, Sasaki (1951): 3 ranges. One-Pion-Exchange (OPE): o.k. Multi-pion exchanges: Problems! Taketani, Machida, Onuma (1952); Brueckner, Watson (1953). Quotes by Bethe (1953) and Goldberger (1960) “Pion Theories” Discovery of the pion in cosmic ray (1947) and in the Berkeley Cyclotron Lab (1948). Nobelprize awarded to Yukawa (1949). 1940’s The first pion period: results in a disaster

17 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 17 Phase II: The meson period 1960’s Many pions = multi-pion resonances: One-Boson-Exchange Model

18 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 18 Phase II: The meson period 1960’s Many pions = multi-pion resonances: One-Boson-Exchange Model

19 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 19 Phase II: The meson period 1960’s Many pions = multi-pion resonances: One-Boson-Exchange Model 1970’s Refined Meson Theories Sophisticated models for two-pion exchange: Paris Potential (Lacombe et al., PRC 21, 861 (1980)) Bonn potential (Machleidt et al., Phys. Rep. 149, 1 (1987))

20 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 20 The exponential tail of phase II (or the epigone period of meson theory) 1980’s Nijmegen: We need more precision!!! “A χ ²/dat of ≈ 2 is not good enough, it has to be 1.0” 1990’s 1993: The high-precision Nijmegen phase shift analysis 1994-2001: High-precision NN potentials: Nijmegen I, II, ’93, Reid93 (Stoks et al. 1994) Argonne V18 (Wiringa et al, 1995) CD-Bonn (Machleidt et al. 1996, 2001)

21 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 21 Gell-Mann Zweig 21 1960’s Many pions = multi-pion resonances: One-Boson-Exchange Model Gell-Mann and Zweig (1963): 3 quarks!

22 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 22 1980’s Nuclear physicists discover QCD: Quark cluster models. 1990 – today Nuclear physicists discover Effective Field Theory (EFT): Weinberg (1990); Ordonez, Ray, van Kolck (1994/96). Another “pion theory”; but now right: constrained by chiral symmetry Phase III: The QCD/EFT period

23 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 23 1980’s Nijmegen: We need more precision!!! 1990’s 1993: The high-precision Nijmegen phase shift analysis 1994-2001: High-precision NN potentials: Nijmegen I, II, ’93, Reid93; Argonne V18; CD-Bonn. 1980’s Nuclear physicists discover QCD: Quark cluster models. 1990 - today Nuclear physicists discover Effective Field Theory (EFT): Weinberg (1990); Ordonez, Ray, van Kolck (1994/96). Another “pion theory”; but now right: constrained by chiral symmetry Phase III: The QCD/EFT period The second pion period: No disaster!

24 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 24 Properties of the nuclear force Finite range Intermediate-range attraction Short-range repulsion (“hard core”) Spin-dependent non-central forces: - Tensor force - Spin-orbit force Charge independence

25 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 25 Finite range Comparison of the binding energies of show that the nuclear force is of finite range (1-2 fm) and very strong within that range (Wigner, 1933). “Saturation”. Nuclei with A>4 show saturation: Volume and binding energies of nuclei are proportional to the mass number A.

26 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 26 Intermediate-range attraction Nuclei are bound. The average distance between nucleons in nuclei is about 2 fm which must roughly correspond to the range of the attractive force.

27 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 27 Short-range repulsion (“hard core”) Analyze 1S0 phase shifts and compare to 1D2 phase shifts.

28 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 28 Non-central forces Tensor Force: First evidence from the deuteron Deuteron

29 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 29 Tensor force, cont’d

30 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 30 Tensor force, cont’d

31 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 31 Non-central forces Spin-Orbit Force Nucleus or proton right left Proton 1 Proton 2

32 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 32 Summary: Most important parts of the nuclear force Short Inter- mediate Long range Tensor force Spin-orbit force Central force Taketani, Nakamura, Sasaki (1951): 3 ranges

33 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 33 Charge-independence After correcting for the electromagnetic interaction, the forces between nucleons (pp, nn, or np) in the same state are almost the same. “Almost the same”: Charge-independence is slightly broken. Notation: Equality between the pp and nn forces: Charge symmetry. Equality between pp/nn force and np force: Charge independence. Better notation: Isospin symmetry; invariance under rotations in isospin space.

34 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 34 Since the scattering length is a magnifying glass on the interaction, charge-independence breaking (CIB) is seen most clearly in the different scattering lengths of pp, nn, and np low-energy scattering. Charge-symmetry breaking (CSB) - after electromagnetic effects have been removed: Charge-independence breaking: Evidence Charge-independence breaking (CIB):

35 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 35 Phenomenological descriptions Symmetries and the general expression for the NN potential Historically important examples of phenomenological NN potentials

36 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 36 The symmetries Translation invariance Galilean invariance Rotation invariance Space reflection invariance Time reversal invariance Invariance under the interchange of particle 1 and 2 Isospin symmetry Hermiticity

37 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 37 Most general two-body potential under those symmetries (Okubo and Marshak, Ann. Phys. 4, 166 (1958)) with central tensor quadratic spin-orbit spin-orbit another tensor

38 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 38 Potentials which are based upon the operator structure shown on the previous slide (but may not include all operators shown or may include additional operators) are called “Phenomenological Potentials”. Some historically important examples are given below. Gammel-Thaler potential ( Phys. Rev. 107, 291, 1339 (1957)), hard-core. Hamada-Johnston potential (Nucl. Phys. 34, 382 (1962)), hard core. Reid potential (Ann. Phys. (N.Y.) 50, 411 (1968)), soft core. Argonne V14 potential (Wiringa et al., Phys. Rev. C 29, 1207 (1984)), uses 14 operators. Argonne V18 potential (Wiringa et al., Phys. Rev. C 51, 38 (1995)), uses 18 operators.

39 R. MachleidtNuclear Forces - Lecture 1 History, Facts, Phen. (CNSSS13) 39 End Lecture 1

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