FermiGasy. W. Udo Schröder, 2004 FermiGas Model 2 Particles in Ideal 1D Box Approximate picture: independent particles in mean field produced by interactions.

Slides:



Advertisements
Similar presentations
Compound Nucleus Reactions
Advertisements

Accelerator Physics, JU, First Semester, (Saed Dababneh).
These describe matter. Starts with a “p”
Stellar Structure Section 5: The Physics of Stellar Interiors Lecture 11 – Total pressure: final remarks Stellar energy sources Nuclear binding energy.
The role of the isovector monopole state in Coulomb mixing. N.Auerbach TAU and MSU.
Kernfysica: quarks, nucleonen en kernen
8-1 RFSS: Lecture 8 Nuclear Force, Structure and Models Readings: §Nuclear and Radiochemistry: Chapter 10 (Nuclear Models) §Modern Nuclear Chemistry: Chapter.
Binding energy in atoms and nuclei [Sec. 4.1 Dunlap]
Atomic Nuclear1 Atomic Nuclei Radius of an atom ~ 10 –10 m (Å, Angstrom unit) Radius of a nucleus ~ 10 –15 m (fm, fermi or Femto-meter) Atomic nuclei are.
P461 - Nuclei I1 Properties of Nuclei Z protons and N neutrons held together with a short-ranged force  gives binding energy P and n made from quarks.
Nov 2006, Lecture 2 Nuclear Physics Lectures, Dr. Armin Reichold 1 Lecture 2 The Semi Empirical Mass Formula SEMF.
(taken from H-J. Wolesheima,
Degenerate Fermi Gas.
Week 1: Basics Reading: Jensen 1.6,1.8,1.9. Two things we focus on DFT = quick way to do QM – 200 atoms, gases and solids, hard matter, treats electrons.
BASIC CONCEPTS.  Summary-1  The net nuclear charge in a nuclear species is equal to + Ze, where Z is the atomic number and e is the magnitude.
(and some things about the weak interaction)
Fermi Gas Model Heisenberg Uncertainty Principle Particle in dx will have a minimum uncertainty in p x of dp x dx pxpx Next particle in dx will have.
Single Particle Energies
Stellar Interior. Solar Facts Radius: –R  = 7  10 5 km = 109 R E Mass : –M  = 2  kg –M  = 333,000 M E Density: –   = 1.4 g/cm 3 –(water is.
Lecture 25 Practice problems Boltzmann Statistics, Maxwell speed distribution Fermi-Dirac distribution, Degenerate Fermi gas Bose-Einstein distribution,
Stellar Structure Section 5: The Physics of Stellar Interiors Lecture 10 – Relativistic and quantum effects for electrons Completely degenerate electron.
P460 - Quan. Stats. III1 Boson and Fermion “Gases” If free/quasifree gases mass > 0 non-relativistic P(E) = D(E) x n(E) --- do Bosons first let N(E) =
P461 - Nuclei I1 Properties of Nuclei Z protons and N neutrons held together with a short-ranged force  gives binding energy P and n made from quarks.
Isospin Charge independence Accordingly, one can develop a formalism that encompasses this concept. Strong empirical empirical evidence to imply that:
FermiGasy. W. Udo Schröder, 2005 Pairing Energy 2 1 Nucleon Pair Outside Closed Shells 2 s/1 d 1 p 1 s 2 6 2/10 18 O neutrons 18 O: 2 neutrons outside.
Nuclear and Radiation Physics, BAU, 1 st Semester, (Saed Dababneh). 1 Nuclear Reactions Categorization of Nuclear Reactions According to: bombarding.
NUCLEAR STRUCTURE PHENOMENOLOGICAL MODELS
Nucleons & Nuclei a quick guide to the real essentials in the subject which particle and nuclear physicists won’t tell you.
W. Udo Schröder, 2007 Semi-Classical Reaction Theory 1.
Nucleon-Nucleon Forces
The Interior of Stars I Overview Hydrostatic Equilibrium
Exam I results.
Nuclear Force Proton – Nucleon and Neutron – Nucleon Interactions.
FermiGasy. W. Udo Schröder, 2005 Angular Momentum Coupling 2 Addition of Angular Momenta    
Lecture 21. Grand canonical ensemble (Ch. 7)
FermiGasy. W. Udo Schröder, 2005 Angular Momentum Coupling 2 Addition of Angular Momenta    
1 Applications:  Environmental studies  Earth and planetary science  Life science (nuclear medicine)  Material science  Separation technology  Hot-atom.
Nuclear Level Density 1.What we know, what we do not know, and what we want to know 2.Experimental techniques to study level densities, what has been done.
Experimental evidence for closed nuclear shells Neutron Proton Deviations from Bethe-Weizsäcker mass formula: mass number A B/A (MeV per nucleon)
Lecture 16: Beta Decay Spectrum 29/10/2003 (and related processes...) Goals: understand the shape of the energy spectrum total decay rate sheds.
Lecture 1 & 2 © 2015 Calculate the mass defect and the binding energy per nucleon for a particular isotope.Calculate the mass defect and the binding.
Microscopic Modeling of Supernova Matter Igor Mishustin FIAS, J. W. Goethe University, Frankfurt am Main, Germany and National Research Center “Kurchatov.
 Nature of nuclear forces, cont.  Nuclear Models lecture 3&4.
NUCLEAR LEVEL DENSITIES NEAR Z=50 FROM NEUTRON EVAPORATION SPECTRA IN (p,n) REACTION B.V.Zhuravlev, A.A.Lychagin, N.N.Titarenko State Scientific Center.
Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran.
The nuclear mean field and its symmetries W. Udo Schröder, 2011 Mean Field 1.
The Nuclear Shell Model A Review of The Nuclear Shell Model By Febdian Rusydi.
Lecture 21: On to Finite Nuclei! 20/11/2003 Review: 1. Nuclear isotope chart: (lecture 1) 304 isotopes with t ½ > 10 9 yrs (age of the earth) 177.
Nuclear and Radiation Physics, BAU, 1 st Semester, (Saed Dababneh). 1 Shell model Notes: 1. The shell model is most useful when applied to closed-shell.
July 29-30, 2010, Dresden 1 Forbidden Beta Transitions in Neutrinoless Double Beta Decay Kazuo Muto Department of Physics, Tokyo Institute of Technology.
Z.Q. Feng( 冯兆庆 ), W.F. Li( 李文飞 ), Z.Y. Ming( 明照宇 ), L.W. Chen( 陈列文 ), F. S. Zhang ( 张丰收 ) Institute of Low Energy Nuclear Physics Beijing Normal University.
Depletion of the Nuclear Fermi Sea  Motivation  General properties momentum distributions.  Single particle spectral functions at zero and finite Temperature.
Preequilibrium Reactions Dr. Ahmed A.Selman. The exciton model was proposed by Griffin in 1966 in order to explain the nuclear emission from intermediate.
Gross Properties of Nuclei
Sizes. W. Udo Schröder, 2011 Nuclear Spins 2 Intrinsic Nuclear Spin Nuclei can be deformed  can rotate quantum mech.  collective spin and magnetic effects.
Nuclear and Radiation Physics, BAU, 1 st Semester, (Saed Dababneh). 1 Electromagnetic moments Electromagnetic interaction  information about.
Nuclear Physics, JU, Second Semester,
Variational Multiparticle-Multihole Configuration Mixing Method with the D1S Gogny force INPC2007, Tokyo, 06/06/2007 Nathalie Pillet (CEA Bruyères-le-Châtel,
Fermi Gas. Particle physics BosonFermion name spin charge mass.
W. Udo Schröder, 2005 Gamma Decay 1. W. Udo Schröder, 2005 Gamma Decay 2 Photons Photons: generated by moving charge distributions. Distributions can.
Nuclear Phenomenology 3C24 Nuclear and Particle Physics Tricia Vahle & Simon Dean (based on Lecture Notes from Ruben Saakyan) UCL.
Semi-Empirical Mass Formula part II Quantum Terms
Pairing Evidence for pairing, what is pairing, why pairing exists, consequences of pairing – pairing gap, quasi-particles, etc. For now, until we see what.
Structure and dynamics from the time-dependent Hartree-Fock model
Content Heavy ion reactions started fragmenting nuclei in the 1980’s. Its study taught us that nuclear matter has liquid and gaseous phases, phase.
CHAPTER 12 The Atomic Nucleus
Neutron Stars Aree Witoelar.
Nuclear Chemistry CHEM 396 Chapter 4, Part B Dr. Ahmad Hamaed
Angular Momentum Coupling
Representations and Algebra
Presentation transcript:

FermiGasy

W. Udo Schröder, 2004 FermiGas Model 2 Particles in Ideal 1D Box Approximate picture: independent particles in mean field produced by interactions of all nucleons  calculate single-particle spectrum  approximate potential (first neglect V Coulomb ) Average Potential V(x) a x  1 (x)  2 (x)  3 (x)  n / 1  1 (x),  2 (x),  3 (x)

W. Udo Schröder, 2004 FermiGas Model 3 Particles in Ideal Multi-D Box State Space n i = 1,2,3,.. i=x,y,z  2D x y a x =a y =a z =100 nxnx nyny nznz 

W. Udo Schröder, 2004 FermiGas Model 4 Density of Fermi Gas States nxnx nznz  3D box, side length a, volume V = a 3 Every point on 3D-integer grid in p-space represents one state n»1  continuous approximation How many states dn in {p, p+dp}  {, +d}? dn/d  = A nucleons FF empty

W. Udo Schröder, 2004 FermiGas Model 5 The Fermi Energy dn/d  = A nucleons FF empty  A = matter density Fermi energy  (nucleon density) 2/3  Fast nucleons in dense matter Fill all single-particle states with 4 nucleons each (spin, isospin up/down)  degenerate FG Nuclear matter:  F = 37 MeV  A = 0.16 fm -3 k F = 1.36 fm -1 p F =  k F =268MeV/c Mean field potential U 0 =  F + B/A = 45 MeV

W. Udo Schröder, 2004 FermiGas Model 6 Total Energy r 0 = ( ) fm Treat all nucleons same with 2 s x 2  qu. numbers, degenerate states

W. Udo Schröder, 2004 FermiGas Model 7 2-Component Fermi Gas FF VnVn VpVp r r Mix of 2 independent (n,p) gases Protons feel Coulomb potential V Coul In real nuclei  F (N)   F (Z) Otherwise conversion ( decay) n  p  Nuclei have N > Z pxpx pypy pF=kFpF=kF Ground state: degenerate FG (T=0) Excited state: non degenerate FG (T≠0) pxpx pypy T Ground State

W. Udo Schröder, 2004 FermiGas Model 8 r 0 = 1.4 fm

W. Udo Schröder, 2004 FermiGas Model 9 Asymmetry Energy This is the origin of the asymmetry energy in the LDM !

Seminar: Statistical Decay of Complex Systems (Nuclei) 1.Nuclear Models: The Fermi Gas 2.Density of states of A-body system Temperature concept and level density 3.Spin and structure dependence of level densities 4.Weisskopf model of statistical decay Examples and applications 5.Hauser-Feshbach model 6.Dynamical effects 7.Pre-equilibrium decay 8.Compound nucleus reactions 9.Multi-fragment decay