[1]:
%matplotlib inline
# change scale of all figures to make them bigger
import matplotlib as mpl
mpl.rcParams['figure.dpi']=100

General reminder: Anderson impurity model and CTHYB solver

In the Anderson impurity model, we decompose the full lattice problem into an interacting site (‘impurity’) hybridised to a bath:

b2283bcaf8ee4663913c98af793ab878

with the Hamiltonian :nbsphinx-math:`begin{align*}

H = & color{red}{H_{rm imp}} + color{darkgreen}{H_{rm hyb}} + color{blue}{H_{rm bath}} \ color{red}{H_{rm imp}} = & sum_{alpha beta} epsilon_{alpha beta} c^{dagger}_{alpha} c_{beta} + sum_{alpha beta gamma delta} U_{alpha beta gamma delta} c^{dagger}_{alpha} c^{dagger}_{beta} c_{delta} c_{gamma} \ color{darkgreen}{H_{rm hyb}} = & sum_{alpha nu k} (V_{alpha nu k} c^{dagger}_{alpha} d_{nu k} + h.~c.) \ color{blue}{H_{rm bath}} = & sum_{nu k} epsilon_{nu k} d^{dagger}_{nu k} d_{nu k}.

end{align*}`

The basic idea behind the CTHYB algorithm is to solve the impurity model by diagrammatically expanding the partition function \(Z\) in orders of the hybridization function. The resulting diagrams are then sampled stochastically using Monte Carlo while measuring quantities of interest, such as the Green’s function. Contrary to the IPT solver, CTHYB yields, within statistical error-bars, the exact solution of the impurity model.

The CTHYB solver needs two pieces of information as input from the user: - the interacting Hamiltonian, \(H_{\rm int} = \sum_{\alpha \beta \gamma \delta} U_{\alpha \beta \gamma \delta} c^{\dagger}_{\alpha} c^{\dagger}_{\beta} c_{\delta} c_{\gamma}\), - the non-interacting Green’s function, \(G_0(i\omega_n)\), from which the energy levels \(\epsilon\) and hybridization function are deduced.

The TRIQS/CTHYB impurity solver

In this notebook, we will see how to use the CTHYB impurity solver (documentation here). We will take the example of a single-orbital Anderson impurity model with a local Coulomb interaction on the impurity orbital

\[H_\mathrm{int} = U n_\mathrm{\uparrow} n_\mathrm{\downarrow}\]

The non-interacting Green’s function is

\[G_0(i\omega_n) = \frac{1}{i\omega_n - \epsilon_d - V^2 \Gamma(i\omega_n)}\]

and \(\Gamma\) is the Green’s function of a flat conduction bath.

Setting up the impurity solver

Here is an example showing how to construct an impurity solver and run it on a single-orbital Anderson impurity model. Wait until the calculation is over before going on (see the “Kernel busy” solid circle on the top right).

[2]:
from triqs.gf import *
from triqs.operators import *
from triqs_cthyb import Solver

V = 1.0           # Hybridization strength
U = 4.0           # Local (on-site) Coulomb interaction
epsilon_d = 0.2   # Orbital energy level
beta = 20         # Inverse temperature

# Construct the impurity solver
S = Solver(beta = beta, gf_struct = [('up',1), ('down',1)] )

# Define the non-interacting Green's function
S.G0_iw << inverse(iOmega_n - epsilon_d - V**2 * Flat(1.0))

# Define the interacting Hamiltonian
h_int = U * n('up',0) * n('down',0)

# Solve the impurity problem for a given local Hamiltonian.
S.solve(h_int = h_int,
        length_cycle = 10,         # Number of steps between each measurement
        n_warmup_cycles = 5000,    # Number of warmup cycles
        n_cycles = 50000           # Number of QMC cycles
       )
Warning: could not identify MPI environment!
Starting serial run at: 2023-08-28 17:49:03.483848

╔╦╗╦═╗╦╔═╗ ╔═╗  ┌─┐┌┬┐┬ ┬┬ ┬┌┐
 ║ ╠╦╝║║═╬╗╚═╗  │   │ ├─┤└┬┘├┴┐
 ╩ ╩╚═╩╚═╝╚╚═╝  └─┘ ┴ ┴ ┴ ┴ └─┘

The local Hamiltonian of the problem:
0.2*c_dag('down',0)*c('down',0) + 0.2*c_dag('up',0)*c('up',0) + 4*c_dag('down',0)*c_dag('up',0)*c('up',0)*c('down',0)
Using autopartition algorithm to partition the local Hilbert space
Found 4 subspaces.

Warming up ...
17:49:03 100% ETA 00:00:00 cycle 4999 of 5000



Accumulating ...
17:49:03  19% ETA 00:00:00 cycle 9760 of 50000
17:49:04 100% ETA 00:00:00 cycle 49999 of 50000


[Rank 0] Collect results: Waiting for all mpi-threads to finish accumulating...
[Rank 0] Timings for all measures:
Measure               | seconds
Auto-correlation time | 0.00566571
Average order         | 0.000908685
Average sign          | 0.000881916
G_tau measure         | 0.0114234
Total measure time    | 0.0188797
[Rank 0] Acceptance rate for all moves:
Move set Insert two operators: 0.0512121
  Move  Insert Delta_up: 0.0513189
  Move  Insert Delta_down: 0.0511046
Move set Remove two operators: 0.0509981
  Move  Remove Delta_up: 0.0513082
  Move  Remove Delta_down: 0.0506868
Move set Insert four operators: 0.00488083
  Move  Insert Delta_up_up: 0.00562934
  Move  Insert Delta_up_down: 0.0033534
  Move  Insert Delta_down_up: 0.00373554
  Move  Insert Delta_down_down: 0.00676994
Move set Remove four operators: 0.00496258
  Move  Remove Delta_up_up: 0.00575551
  Move  Remove Delta_up_down: 0.0038171
  Move  Remove Delta_down_up: 0.00347195
  Move  Remove Delta_down_down: 0.00682145
Move  Shift one operator: 0.689225
[Rank 0] Warmup lasted: 0.0479879 seconds [00:00:00]
[Rank 0] Simulation lasted: 0.507693 seconds [00:00:00]
[Rank 0] Number of measures: 50000
Total number of measures: 50000
Average sign: 1
Average order: 14.716
Auto-correlation time: 86.6392

Let’s try to explain the different lines of the script above. To construct the solver all that is needed is the inverse temperature \(\beta\) and a list that describes the block structure of the Green’s function. This is the gf_struct keyword. In this specific case, there are two (disconnected) blocks up and down and each containing only one orbital with the index 0. This is what is described by gf_struct.

Then, the member S.G0_iw of the solver is initialized. This Green’s function will be used as the non-interacting Green’s function when the solver starts.

The final step is to run the solver with the solve method. It has a certain number of parameters:

  • h_int: This is the interacting Hamiltonian (i.e. the quartic terms in the local Hamiltonian, those with 4 operators) solved for in the Monte Carlo. It is defined using the operators that we have seen in the previous notebook. Important: the name of the indices in the operators have to be compatible with the gf_struct that was used in the construction of the solver.

  • length_cycle: This is the number of steps at which measurements, e.g. of G_tau, are made to ensure data is decorrelated.

  • n_warmup_cycles: The number of cycles used to thermalize the system.

  • n_cycles: This is the number of Monte Carlo cycles, which is also the number of measures of the Green’s function.

So a calculation will have a Markov chain of length length_cycle * (n_warmup_cycles + n_cycles).

When the run is over, the outputs of the solver are:

  • S.G_tau: The Green’s function in imaginary time of the system.

  • S.G_iw: The Green’s function in Matsubara frequency of the system.

  • S.Sigma_iw: The self-energy in Matsubara frequency.

Tips for advanced use: - For some more complex standard Hamiltonians, the library provides functions that can be used to construct h_int. See the operators section of the TRIQS documentation. - It is likely that for more involved calculations, you will have more parameters that you can adjust. See the online CTHYB documentation. - If you have many more parameters, it can be beneficial to set the parameters in a dictionary at the top of your script and simply pass the dictionary to solve using Python keyword arguments:

p = {}                        # Initialize an empty Python dictionary
p['length_cycle'] = 10        # Fill the dictionary with parameters
p['n_warmup_cycles'] = 5000
p['n_cycles'] = 50000

S.solve(h_int = h_int, **p)   # The dictionary contents will be unrolled as arguments to the solve function

Visualizing the imaginary time sampled \(G(\tau)\)

Fundamentally the cthyb solver samples diagrams of the partition function. The imaginary time impurity Green’s function is then measured by removing individual hybridization lines, yielding samples at randomly chosen time-points. The samples at then gathered into bins obtained by splitting the interval \([0,\beta)\) into n_tau pieces.

We can visualize the result by plotting the raw data. The noise for each bin is inversely proportional the number of samples that fall into it. By increasing the bin-size we can reduce the noise level (but we introduce a systematic binning error). This is achieved with the rebinning_tau function

[3]:
from triqs.plot.mpl_interface import *

oplot(S.G_tau['up'].real, '-', c='C0', label='raw MC data')

G_imp_rebinned = S.G_tau['up'].rebinning_tau(new_n_tau=500)
oplot(G_imp_rebinned.real, '-', c='C1', label='rebinned')

plt.legend(loc='lower right')
plt.show()
../../../../_images/userguide_python_tutorials_ModelDMFT_02-Introduction_to_the_CTHYB_solver_6_0.png

Visualizing the Matsubara-frequency results

We can also plot the results on the Matsubara axis and see how our statistics look in terms of the resulting noise. The solver automatically Fourier transforms S.G_tau to the Matsubara axis after finishing sampling, and the resulting Green’s function can be accessed as S.G_iw:

[4]:
oplot(S.G_iw, 'o')
plt.xlim(0,20)
plt.show()
../../../../_images/userguide_python_tutorials_ModelDMFT_02-Introduction_to_the_CTHYB_solver_8_0.png
[5]:
oplot(S.Sigma_iw, '-o')
plt.xlim(0,20)
plt.ylim(-1.0,2.0)
plt.show()
../../../../_images/userguide_python_tutorials_ModelDMFT_02-Introduction_to_the_CTHYB_solver_9_0.png

The large oscillations in the self-energy are due to a bad statistics in the Monte Carlo.

Exercise


Increase and decrease the number of Monte Carlo cycles to see its effect on the quality of the self-energy.