Supplement: Statistical Physics

Size: px

Start display at page:

Download "Supplement: Statistical Physics"

Marshall Park
5 years ago
Views:

1 Supplement: Statistical Physics

2 Fitting in a Box. Counting momentum states with momentum q and de Broglie wavelength λ = h q = 2π h q In a discrete volume L 3 there is a discrete set of states that satisfy periodic boundary conditions We will hereafter set h = c = 1 As in Fourier analysis e 2πix/λ = e iqx = e iq(x+l) e iql = 1

3 Fitting in a Box Periodicity yields a discrete set of allowed states Lq = 2πm i, m i = 1, 2, 3... q i = 2π L m i In each of 3 directions m xi m yj m zk d 3 m The differential number of allowed momenta in the volume d 3 m = ( ) 3 L d 3 q 2π

4 Density of States The total number of states allows for a number of internal degrees of freedom, e.g. spin, quantified by the degeneracy factor g Total density of states: dn s V = g V d3 m = g (2π) 3 d3 q If all states were occupied by a single particle, then particle density n s = N s V = 1 g dn s = V (2π) 3 d3 q

5 Distribution Function The distribution function f quantifies the occupation of the allowed momentum states n = N V = 1 g fdn s = V (2π) 3 fd3 q f, aka phase space occupation number, also quantifies the density of particles per unit phase space dn/( x) 3 ( q) 3 For photons, the spin degeneracy g = 2 accounting for the 2 polarization states Energy E(q) = (q 2 + m 2 ) 1/2 Momentum frequency q = 2π/λ = 2πν = ω = E (where m = 0 and λν = c = 1)

6 Bulk Properties Integrals over the distribution function define the bulk properties of the collection of particles Number density Energy density where E 2 = q 2 + m 2 Momentum density n(x, t) N V = g ρ(x, t) = g (ρ + p)v(x, t) = g d 3 q (2π) 3 f d 3 q (2π) 3 E(q)f d 3 q (2π) 3 qf

7 Bulk Properties. Pressure: particles bouncing off a surface of area A in a volume spanned by L x : per momentum state vx v p q = F A = N part q A t ( q = 2 q x, t = 2L x /v x, ) = N part V q x v x = N part q v V 3 (v = γmv/γm = q/e) = N part V q 2 3E Lx

8 Bulk Properties So that summed over occupied momenta states p(x, t) = g d 3 q (2π) 3 q 2 3E(q) f Pressure is just one of the quadratic in q moments, in particular the isotropic one The remaining 5 components are the anisotropic stress (vanishes in the background) π i j(x, t) = g d 3 q 3q i q j q 2 δ i j f (2π) 3 3E(q) We shall see that these are related to the 5 quadrupole moments of the angular distribution

9 Bulk Properties These are more generally the components of the stress-energy tensor T µ d 3 q q µ q ν ν = g (2π) 3 E(q) f 0-0: energy density 0-i: momentum density i i: pressure i j: anisotropic stress In the FRW background cosmology, isotropy requires that there be only a net energy density and pressure

10 Equilibrium Thermal physics describes the equilibrium distribution of particles for a medium at temperature T Expect that the typical energy of a particle by equipartition is E T, so that f eq (E/T,?) in equilibrium Must be a second variable of import. Number density n = g d 3 q (2π h) 3 f eq(e/t ) =? n(t ) If particles are conserved then n cannot simply be a function of temperature. The integration constant that concerns particle conservation is called the chemical potential. Relevant for photons when creation and annihilation processes are ineffective

11 Temperature and Chemical Potential Fundamental assumption of statistical mechanics is that all accessible states have an equal probability of being populated. The number of states G defines the entropy S(U, N, V ) = ln G where U is the energy, N is the number of particles and V is the volume When two systems are placed in thermal contact they may exchange energy, particles, leading to a wider range of accessible states G(U, N, V ) = U 1,N 1 G 1 (U 1, N 1, V 1 )G 2 (U U 1, N N 1, V 2 ) The most likely distribution of U 1 and U 2 is given for the maximum dg/du 1 = 0 ( ) ( ) G1 G2 G 2 du 1 + G 1 du 2 = 0 du 1 + du 2 = 0 U 1 N 1,V 1 U 2 N 2,V 2

12 Temperature and Chemical Potential Or equilibrium requires ( ) ln G1 U 1 N 1,V 1 = ( ) ln G2 U 2 N 2,V 2 1 T which is the definition of the temperature (equal for systems in thermal contact) Likewise define a chemical potential µ for a system in diffusive equilibrium ( ) ( ) ln G1 ln G2 N 1 U 1,V 1 = N 2 U 2,V 2 µ T defines the most likely distribution of particle numbers as a system with equal chemical potentials: generalize to multiple types of particles undergoing chemical reaction law of mass action i µ idn i = 0

13 Temperature and Chemical Potential Equivalent definition: the chemical potential is the free energy cost associated with adding a particle at fixed temperature and volume µ = F N T,V, F = U T S free energy: balance between minimizing energy and maximizing entropy S Temperature and chemical potential determine the probability of a state being occupied if the system is in thermal and diffusive contact with a large reservoir at temperature T

14 Gibbs or Boltzmann Factor Suppose the system has two states unoccupied N 1 = 0, U 1 = 0 and occupied N 1 = 1, U 1 = E then the ratio of probabilities in the occupied to unoccupied states is given by Taylor expand P = exp[ln G res(u E, N 1, V )] exp[ln G res (U, N, V )] ln G res (U E, N 1, V ) ln G res (U, N, V ) E T + µ T This is the Gibbs factor. P exp[ (E µ)/t ]

15 Gibbs or Boltzmann Factor More generally the probability of a system being in a state of energy E i and particle number N i is given by the Gibbs factor P (E i, N i ) exp[ (E i µn i )/T ] Unlikely to be in an energy state E i T mitigated by the number of particles Dropping the diffusive contact, this is the Boltzmann factor

16 Thermal & Diffusive Equilibrium A gas in thermal & diffusive contact with a reservoir at temperature T Probability of system being in state of energy E i and number N i (Gibbs Factor) P (E i, N i ) exp[ (E i µn i )/T ] where µ is the chemical potential (defines the free energy cost for adding a particle at fixed temperature and volume) Chemical potential appears when particles are conserved CMB photons can carry chemical potential if creation and annihilation processes inefficient, as they are after t 1yr.

17 Distribution Function Mean occupation of the state in thermal equilibrium f Ni P (E i, N i ) P (Ei, N i ) where the total energy is related to the particle energy as E i = N i E (ignoring zero pt) Density of (energy) states in phase space makes the net spatial density of particles n = g d 3 p (2π) 3 f where g is the number of spin states

18 Fermi-Dirac Distribution For fermions, the occupancy can only be N i = 0, 1 f = P (E, 1) P (0, 0) + P (E, 1) = e (E µ)/t = 1 + e (E µ)/t 1 e (E µ)/t + 1 In the non-relativistic, non-degenerate limit E = (q 2 + m 2 ) 1/2 m and m T so the distribution is Maxwell-Boltzmann q 2 m f = e (m µ)/t e q2 /2mT = e (m µ)/t e mv2 /2T

19 Bose-Einstein Distribution For bosons each state can have multiple occupation, d dµ/t N=0 f = (e (E µ)/t ) N with x N = 1 N=0 (e (E µ)/t ) N 1 x N=0 1 = e (E µ)/t 1 Again, non relativistic distribution is Maxwell-Boltzmann f = e (m µ)/t e q2 /2mT = e (m µ)/t e mv2 /2T with a spatial number density n = ge (m µ)/t = ge (m µ)/t ( mt 2π d 3 q /2mT (2π) 3 e q2 ) 3/2

20 Ultra-Relativistic Bulk Properties Chemical potential µ = 0, ζ(3) Number density n boson = gt 3 ζ(3) ζ(n + 1) 1 π 2 n! n fermion = 3 3 ζ(3) gt 4 π 2 Energy density 0 xn dx e x 1 ρ boson = gt π2 ζ(4) = gt π2 30 ρ fermion = 7 8 gt 4 3 π ζ(4) = 7 4 π2 gt Pressure q 2 /3E = E/3 p = ρ/3, w r = 1/3

21 Boltzmann Equation Interactions or collisions between particles drive the various distributions to equilibrium through the Boltzmann equation Boltzmann equation is also known as the particle transport or radiative transfer equation Composed of two parts: the free propagation or Liouville equation and the collisions

22 Liouville Equation Liouville theorem: phase space distribution function is conserved along a trajectory in the absence of particle interactions Df Dt = [ t + dq dt q + dx dt ] f = 0 x Expanding universe: de Broglie wavelength of particles stretches q a 1 Homogeneous and isotropic limit f t + dq dt f q = f t H(a) f ln q = 0 Implies energy conservation: dρ/dt = 3H(ρ + p)

23 Boltzmann Equation Boltzmann equation says that Liouville theorem must be modified to account for collisions Heuristically Df Dt = C[f] C[f] = particle sources - sinks Collision term: integrate over phase space of incoming particles, connect to outgoing state with some interaction strength

24 Form: C[f] = 1 E Boltzmann Equation d(phase space)[energy-momentum conservation] M 2 [emission absorption] Matrix element M, assumed T [or CP] invariant (Lorentz invariant) phase space element d(phase space) = Π i g i (2π) 3 d 3 q i Energy conservation: (2π) 4 δ (4) (q 1 + q ) 2E i

25 Boltzmann Equation Emission - absorption term involves the particle occupation of the various states For concreteness: take f to be the photon distribution function Interaction (γ + i µ); sums are over all incoming and outgoing other particles photon f f i other i states absorption emission M f µ f µ other µ states other µ states γ + i µ M photon f f i other i states [emission-absorption] + = boson; = fermion Π i Π µ f µ (1 ± f i )(1 ± f) Π i Π µ (1 ± f µ )f i f

26 Boltzmann Equation Photon Emission: f µ (1 ± f i )(1 + f) f µ : proportional to number of emitters (1 ± f i ): if final state is occupied and a fermion, process blocked; if boson the process enhanced (1 + f): final state factor for photons: 1 : spontaneous emission (remains if f = 0); +f : stimulated and proportional to the occupation of final photon Photon Absorption: (1 ± f µ )f i f (1 ± f µ ): if final state is occupied and fermion, process blocked; if boson the process enhanced f i : proportional to number of absorbers f: proportional to incoming photons

27 Boltzmann Equation If interactions are rapid they will establish an equilibrium distribution where the distribution functions no longer change C[f eq ] = 0 Solve by inspection Π i Π µ f µ (1 ± f i )(1 ± f) Π i Π µ (1 ± f µ )f i f = 0 Try f a = (e E a/t 1) 1 so that (1 ± f a ) = e E a/t (e E a/t 1) 1 e (E i +E)/T e E µ /T = 0 and energy conservation says E + E i = E µ, so identity is satisfied if the constant T is the same for all species, i.e. are in thermal equilibrium

28 Boltzmann Equation If the interaction does not create or destroy particles then the distribution f eq = (e (E µ)/t 1) 1 also solves the equilibrium equation: e.g. a scattering type reaction γ E + i γ E + j where i and j represent the same collection of particles but with different energies after the scattering (Ei µ i ) + (E µ) = (E j µ j ) + (E µ) since µ i = µ j for each particle Not surprisingly, this is the Fermi-Dirac distribution for fermions and the Bose-Einstein distribution for bosons

29 Boltzmann Equation More generally, equilibrium is satisfied if the sum of the chemical potentials on both sides of the interaction are equal, γ + i ν µi + µ = µ ν i.e. the law of mass action is satisfied If interactions that create or destroy particles are in equilibrium then this law says that the chemical potential will vanish: e.g. γ + e 2γ + e µ e + µ = µ e + 2µ µ = 0 so that the chemical potential is driven to zero if particle number is not conserved in interaction

30 Maxwell Boltzmann Distribution For the nonrelativistic limit E = m q2 /m, nondegenerate limit (E µ)/t 1 so both distributions go to the Maxwell-Boltzmann distribution f eq = exp[ (m µ)/t ] exp( q 2 /2mT ) Here it is even clearer that the chemical potential µ is the normalization parameter for the number density of particles whose number is conserved. µ and n can be used interchangably

31 Poor Man s Boltzmann Equation Non expanding medium f t = Γ (f f eq) where Γ is some rate for collisions Add in expansion in a homogeneous medium f t + dq dt f q = Γ (f f eq) (q a 1 1 q f t H f ln q = Γ (f f eq) dq dt = 1 a da dt = H) So equilibrium will be maintained if collision rate exceeds expansion rate Γ > H

32 Non-Relativistic Bulk Properties Number density n = ge (m µ)/t = ge 4π (2π) 3 (m µ)/t 23/2 2π 0 2 (mt )3/2 = g( mt 2π )3/2 e (m µ)/t Energy density E = m ρ = mn q 2 dq exp( q 2 /2mT ) 0 x 2 dx exp( x 2 ) Pressure q 2 /3E = q 2 /3m p = nt, ideal gas law

33 Ultra-Relativistic Bulk Properties Chemical potential µ = 0, ζ(3) Number density n boson = gt 3 ζ(3) ζ(n + 1) 1 π 2 n! n fermion = 3 3 ζ(3) gt 4 π 2 Energy density 0 x n e x 1 dx ρ boson = gt π2 ζ(4) = gt π2 30 ρ fermion = 7 8 gt 4 3 π ζ(4) = 7 4 π2 gt Pressure q 2 /3E = E/3 p = ρ/3, w r = 1/3

34 First law of thermodynamics Entropy Density ds = 1 T (dρ(t )V + p(t )dv ) so that S V T = 1 T [ρ(t ) + p(t )] = V dρ V T dt S T Since S(V, T ) V is extensive S = V T [ρ(t ) + p(t )] σ = S/V = 1 [ρ(t ) + p(t )] T

35 Entropy Density Integrability condition ds/dv dt = ds/dt dv relates the evolution of entropy density dσ dt = 1 dρ T dt dσ dt = 1 dρ T dt = 1 ln a [ 3(ρ + p)]d T dt d ln σ = 3 d ln a σ a 3 dt dt comoving entropy density is conserved in thermal equilibrium For ultra relativisitic bosons s boson = 3.602n boson ; for fermions factor of 7/8 from energy density. g = bosons g b gf

Set 3: Thermal Physics

Set 3: Thermal Physics Equilibrium Thermal physics describes the equilibrium distribution of particles for a medium at temperature T Expect that the typical energy of a particle by equipartition is E kt,