Classical gas with general dispersion relation For gas of noninteracting particles in d dimensional box with kinetic energy of the form (p)=C|p|s prove the following results: Define =1+(s/d). In an adiabatic process PV=const. The energy is E=NkBT/(1) kB N The entropy is S = ln(PV) + f(N) . 1 The heat capacity ratio is Cp/Cv = . What is the most general form of the function f(N)? Density of a gas inside a rotating box A cylinder of radius R and height H rotates about its axis with a constant angular velocity It contains an ideal classical gas at temperature T. Find the density distribution as function of the distance r from the axis. Note that the Hamiltonian in the rotating frame is H'(p,q; ) = H(p,q) L(p,q) where L(p,q) is the angular momentum. It is conceptually useful to realize that it is formally the Hamiltonian of a charged particle in a magnetic field (=“Coriolis force”) plus centrifugal potential V(r). Explain how this formal equivalence can be used in order to make a “shortcut” in the above calculation. Virial coefficients Find the second virial coefficient B of an ideal Bose gas by evaluating the canonical partition function of two particles. Repeat for an ideal fermion gas. Find the second virial coefficient for: Ideal Bose gas. Ideal Fermi gas. Classical hard sphere gas. Hard Sphere gas Consider a one-dimensional classical gas of N particles in a length L at temperature T. The particles have mass m and interact via a 2-body "hard sphere" interaction (xi is the position of the i-th particle): V(xixj) = ∞ if |xixj|<a, and zero otherwise. Evaluate the exact free energy F(T,L,N). Find the equation of state and identify the first virial coefficient; compare with its direct definition. Show that the energy is E=NkBT/2. Why is there no effect of the interactions on E ? In three dimensions V(|rirj|) is defined as above with r the position vector. Comment on the form of the free energy. 2D coulomb gas N ions of positive charge q and N with negative charge q are constrained to move in a two dimensional square of side L. The interaction energy of charge qi at position ri with another charge qj at rj is qiqj ln|rirj| where qi,qj=±q. a) By rescaling space variables to ri'=Cri, where C is an arbitrary constant, show that the partition function Z(L) satisfies: Z(L)=CN(q 4)Z(CL) . b) Deduce that for low temperatures -1<q2/4, The function Z(CL) for the infinite system (Cinfty) does not exist. What is the origin of this instability? 2 Bose gas for general dispersion relation Consider an ideal Bose gas in d dimensions whose single particle spectrum is given by =C|p|s. Find the condition on s, d for the existence of Bose-Einstein condensation. In particular show that for nonrelativistic particles in two dimensions (s=d=2) the system does not exhibit Bose-Einstein condensation. s E d Show that P= d V and CV(T∞) = s NkB Heat capacity of Bose gas Consider an ideal Bose gas and show that the ratio CP/CV = 3 g1/2(z) g5/2(z) / 2g3/22(z) where z is the fugacity. Why is CP∞ in the condensed phase? Find in the adiabatic equation of state. Note that in general ≠CP/CV . Heat capacity of He4 The specific heat of He4 at low temperatures has the form Cv = AT3 + B(T)exp(-kT) What can you deduce about the excitations of the system? (assume that the density of excitation modes has the form g()~p as ). What would be the form of Cv for a similar system in a two dimensional world? Bose gas in a uniform gravitational field Consider an ideal Bose gas of particles with mass m in a uniform gravitational field of accelaration g. Show that the critical temperature for the Bose-Einstein condensation 8 1 is Tc = Tc0[1+9 ( mgL ) 1/2 ] (3/2) kBTc0 where L is the height of the container, mgL<<kBTc0 and Tc0 =Tc(g=0). [hint: g3/2(z)=g3/2(1)2 ln( z ) + O(ln(z)).] Show that the condensation is accompanied by a discontinuity in the specific heat at 9 mgL 1/2 Tc, with the result CV = (3/2)NkB( ) . 16 kBTc0 [Hint: CV is due to discontinuity in (∂z/∂T)N,V] Quantum Fermi gas in gravitation field of a star Consider a neutron star as non-relativistic gas of non-interacting neutrons of mass m in a spherical symmetric equilibrium configuration. The neutrons are held together by a gravitational potential mMG/r of a heavy object of mass M and radius r0 at the center of the star (G is the gravity constant and r is the distance from the center). Assume that the neutrons are classical (Boltzmann) particles at temperature T and find their density n(r) at r>r0. Is the potential confining? [By definition, for a confining potential there a solution with n(r)0 at r∞] . Next, consider the neutrons as fermions at T=0, and find n(r). Is the potential confining? Extend your result to the case T≠0, and discuss the connection with the Boltzmann limit.