GW - Revision history

Petru Milev at 13:53, 2 May 2025

2025-05-02T13:53:10Z

← Older revision		Revision as of 13:53, 2 May 2025
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	In this tutorial you will learn the basic concepts of the [http://www.yambo-code.eu/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.eu/theory/docs/doc_GW.php GW][[[#strinati\|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G<sub>0</sub>W<sub>0</sub> approximation. Different lecture notes on the GW approach are available in the [[~~../../theory/lectures.php#GW~~\|~~"Lecture Notes"~~ section]].		In this tutorial you will learn the basic concepts of the [http://www.yambo-code.eu/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.eu/theory/docs/doc_GW.php GW][[[#strinati\|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G<sub>0</sub>W<sub>0</sub> approximation. Different lecture notes on the GW approach are available in the [[Lectures\|Lectures section]].

	The tutorial is split in different sections. In the first part we will deal with Hartree-Fock (HF) and the Coulomb-hole and screened-exchange (COHSEX) approximation. Finally in the last section we will discuss dynamical correlation with a Plasmon Pole Approximation (PPA).		The tutorial is split in different sections. In the first part we will deal with Hartree-Fock (HF) and the Coulomb-hole and screened-exchange (COHSEX) approximation. Finally in the last section we will discuss dynamical correlation with a Plasmon Pole Approximation (PPA).

Daniele at 10:29, 23 February 2024

2024-02-23T10:29:22Z

← Older revision		Revision as of 10:29, 23 February 2024
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	<br />		<br />

	Curiosity: What's happen if the PPA fails? Have a look to the tutorial on the [http://www.yambo-code.~~org~~/tutorials/Real_Axis_and_Lifetimes/index.php Real-Axis Integration].		Curiosity: What's happen if the PPA fails? Have a look to the tutorial on the [http://www.yambo-code.eu/tutorials/Real_Axis_and_Lifetimes/index.php Real-Axis Integration].

	== <span id="5">References</span> ==		== <span id="5">References</span> ==

Daniele at 10:28, 23 February 2024

2024-02-23T10:28:54Z

← Older revision		Revision as of 10:28, 23 February 2024
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	where W<sub>p</sub>=W - V.<br />		where W<sub>p</sub>=W - V.<br />
	In order to calculate the COHSEX self-energy with yambo you need first the static screened interaction <code>yambo -b -k hartree</code>. As for the V('''r''') case, also W('''r''','''r'''',E=0) will depend from the number of '''G'''-vectors, and the '''k'''-grid, but this time also the number of conduction bands <code>XsBndsRn</code> will enter in the screening calculation through the polarization function, see [http://www.yambo-code.~~org~~/theory/docs/doc_Xd.php The Interacting response function: Many-Body and TDDFT] section. Notice however that there are not any additional dependence of the self-energy operator from the conduction bands. After you obtained the screened interaction you are ready to build the self-energy operator and solve the corresponding Dyson equation, have a look to the [http://www.yambo-code.~~org~~/theory/docs/doc_GW.php Dyson Equation solvers] in Yambo. In order to get the quasi-particle energies, just do <code>yambo -b -g n -k hartree</code>. After calculation are completed Yambo will produce an output file <code>o.qp</code> which contains the values of the bare and re-normalized energy levels.		In order to calculate the COHSEX self-energy with yambo you need first the static screened interaction <code>yambo -b -k hartree</code>. As for the V('''r''') case, also W('''r''','''r'''',E=0) will depend from the number of '''G'''-vectors, and the '''k'''-grid, but this time also the number of conduction bands <code>XsBndsRn</code> will enter in the screening calculation through the polarization function, see [http://www.yambo-code.eu/theory/docs/doc_Xd.php The Interacting response function: Many-Body and TDDFT] section. Notice however that there are not any additional dependence of the self-energy operator from the conduction bands. After you obtained the screened interaction you are ready to build the self-energy operator and solve the corresponding Dyson equation, have a look to the [http://www.yambo-code.eu/theory/docs/doc_GW.php Dyson Equation solvers] in Yambo. In order to get the quasi-particle energies, just do <code>yambo -b -g n -k hartree</code>. After calculation are completed Yambo will produce an output file <code>o.qp</code> which contains the values of the bare and re-normalized energy levels.

	==== <span id="1">K-points convergence</span> ====		==== <span id="1">K-points convergence</span> ====

Daniele at 10:24, 23 February 2024

2024-02-23T10:24:42Z

← Older revision		Revision as of 10:24, 23 February 2024
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	by the Yambo Team ===		by the Yambo Team ===

	~~[[File:../GW0.png\|G0W0]]~~
	In this tutorial you will learn the basic concepts of the [http://www.yambo-code.eu/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.eu/theory/docs/doc_GW.php GW][[[#strinati\|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G<sub>0</sub>W<sub>0</sub> approximation. Different lecture notes on the GW approach are available in the [[../../theory/lectures.php#GW\|"Lecture Notes" section]].		In this tutorial you will learn the basic concepts of the [http://www.yambo-code.eu/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.eu/theory/docs/doc_GW.php GW][[[#strinati\|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G<sub>0</sub>W<sub>0</sub> approximation. Different lecture notes on the GW approach are available in the [[../../theory/lectures.php#GW\|"Lecture Notes" section]].

Daniele at 10:24, 23 February 2024

2024-02-23T10:24:01Z

← Older revision		Revision as of 10:24, 23 February 2024
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	[[File:../GW0.png\|G0W0]]		[[File:../GW0.png\|G0W0]]
	In this tutorial you will learn the basic concepts of the [http://www.yambo-code.~~org~~/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.~~org~~/theory/docs/doc_GW.php GW][[[#strinati\|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G<sub>0</sub>W<sub>0</sub> approximation. Different lecture notes on the GW approach are available in the [[../../theory/lectures.php#GW\|"Lecture Notes" section]].		In this tutorial you will learn the basic concepts of the [http://www.yambo-code.eu/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.eu/theory/docs/doc_GW.php GW][[[#strinati\|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G<sub>0</sub>W<sub>0</sub> approximation. Different lecture notes on the GW approach are available in the [[../../theory/lectures.php#GW\|"Lecture Notes" section]].

	The tutorial is split in different sections. In the first part we will deal with Hartree-Fock (HF) and the Coulomb-hole and screened-exchange (COHSEX) approximation. Finally in the last section we will discuss dynamical correlation with a Plasmon Pole Approximation (PPA).		The tutorial is split in different sections. In the first part we will deal with Hartree-Fock (HF) and the Coulomb-hole and screened-exchange (COHSEX) approximation. Finally in the last section we will discuss dynamical correlation with a Plasmon Pole Approximation (PPA).
Line 31:		Line 31:
	=== <span id="1">Hartree-Fock</span> ===		=== <span id="1">Hartree-Fock</span> ===

	Now we will study the convergence of the [http://en.wikipedia.~~org~~/wiki/Hartree%E2%80%93Fock_method Hartree-Fock] self energy, respect to the number of '''G'''-vectors and '''k'''-points. Yambo is a plane-wave code, therefore all the operators and wave-functions are expanded as:		Now we will study the convergence of the [http://en.wikipedia.eu/wiki/Hartree%E2%80%93Fock_method Hartree-Fock] self energy, respect to the number of '''G'''-vectors and '''k'''-points. Yambo is a plane-wave code, therefore all the operators and wave-functions are expanded as:
	[[File:orbital.png\|Orbital in plane wave]]		[[File:orbital.png\|Orbital in plane wave]]
	Before you start any calculations we can decide how many '''G'''-vectors you want use to represent your wave-function. By default Yambo will use all of them, and for the present tutorial this is fine, however if you are studying larger systems you would like to reduce them in order to speed-up calculations, you can do it with <code> yambo -i -V RL</code> and then changing the variable <code>MaxGvecs</code> that referees to N<sub>g</sub> in the previous formula.<br />		Before you start any calculations we can decide how many '''G'''-vectors you want use to represent your wave-function. By default Yambo will use all of them, and for the present tutorial this is fine, however if you are studying larger systems you would like to reduce them in order to speed-up calculations, you can do it with <code> yambo -i -V RL</code> and then changing the variable <code>MaxGvecs</code> that referees to N<sub>g</sub> in the previous formula.<br />

Yambowikiadmin at 22:12, 17 February 2017

2017-02-17T22:12:10Z

@@ Line 96: / Line 96: @@
 [[File:gw_sex.png|Screened Exchange]]
 [[File:gw_coh.png|Cuolomb Hole]]
 <br />
@@ Line 140: / Line 141: @@
 Now we will proceed to the calculation of the silicon band gap in G<sub>0</sub>W<sub>0</sub> within PPA. In each section you will be asked to perform several calculations varying the value of the relevant variables involved. More specifically let's consider a typical Yambo input file to calculate GW corrections in the PPA.
-<code> gw0                          # [R GW] GoWo Quasiparticle energy levels ppa                          # [R Xp] Plasmon Pole Approximation HF_and_locXC                 # [R XX] Hartree-Fock Self-energy and Vxc em1d                         # [R Xd] Dynamical Inverse Dielectric Matrix EXXRLvcs= 7            Ry    # [XX] Exchange RL components % QpntsRXp   1 |  8 |                   # [Xp] Transferred momenta % % BndsRnXp    1 | 30 |                 # [Xp] Polarization function bands % NGsBlkXp= 7            Ry    # [Xp] Response block size % LongDrXp  1.000000 | 0.000000 | 0.000000 |        # [Xp] [cc] Electric Field % PPAPntXp= 27.21138     eV    # [Xp] PPA imaginary energy % GbndRnge    1 |  30 |                 # [GW] G[W] bands range % GDamping=  0.10000     eV    # [GW] G[W] damping dScStep=  0.10000      eV    # [GW] Energy step to evalute Z factors DysSolver= &quot;n&quot;               # [GW] Dyson Equation solver (`n`,`s`,`g`) %QPkrange                    # [GW] QP generalized Kpoint/Band indices   1|  8|  1| 10| % %QPerange                    # [GW] QP generalized Kpoint/Energy indices   1|  8| 0.0|-1.0| %</code>
+<code>
 The variables are the same of the COHSEX case plus a new one <code>PPAPntXp</code> that describes the imaginary energy used to fit the Plasmon Pole model.<br />
 Follow the same strategy of the COHSEX case. Enter each k-point folder and type:

Yambowikiadmin: Created page with "=== Basic concepts of the GW approximation
by the Yambo Team === G0W0 In this tutorial you will learn the basic concepts of the [http://www.yambo-co..."

2017-02-17T21:17:26Z

Created page with "=== Basic concepts of the GW approximation by the Yambo Team === [[File:../GW0.png|G0W0]] In this tutorial you will learn the basic concepts of the [http://www.yambo-co..."

New page

=== Basic concepts of the GW approximation 
by the Yambo Team ===

[[File:../GW0.png|G0W0]]
In this tutorial you will learn the basic concepts of the [http://www.yambo-code.org/theory/docs/doc_XX.php Hartree-Fock] and of the [http://www.yambo-code.org/theory/docs/doc_GW.php GW][[[#strinati|6]]] approximations. In particular we will illustrate how to calculate [http://en.wikipedia.org/wiki/Quasiparticle Quasi-Particle] energies with a single shot G0W0 approximation. Different lecture notes on the GW approach are available in the [[../../theory/lectures.php#GW|"Lecture Notes" section]].

The tutorial is split in different sections. In the first part we will deal with Hartree-Fock (HF) and the Coulomb-hole and screened-exchange (COHSEX) approximation. Finally in the last section we will discuss dynamical correlation with a Plasmon Pole Approximation (PPA).

=== The material: Silicon ===

{|
|width="50%"|
'''Bulk Silicon'''
* [http://cst-www.nrl.navy.mil/lattice/struk/a1.html FCC] lattice
* Two atoms per cell (8 electrons)
* Lattice constant 10.183 [a.u.]
* Plane waves cutoff 15 Rydberg
|width="50%"| [[File:si_banddiagram.gif|Silicon Band Structure]]
|}

=== The Tutorial structure ===

Once the tutorial zip file is unzipped the following folder structure will appear

<code> COPYING README Solid_Si/</code> 
with the Solid_Si folder containing 
<code> >ls Solid_Si/ Pwscf/ YAMBO/</code>
* In the Pwscf folder information on the ground state generation are provided. In particular the student will find an input/output directory with input/output files for pw.x. Also a psp folder is provided with the silicon pseudo files.
* The YAMBO folder contains the Yambo input/output files and core databases.

=== Hartree-Fock ===

Now we will study the convergence of the [http://en.wikipedia.org/wiki/Hartree%E2%80%93Fock_method Hartree-Fock] self energy, respect to the number of '''G'''-vectors and '''k'''-points. Yambo is a plane-wave code, therefore all the operators and wave-functions are expanded as:
[[File:orbital.png|Orbital in plane wave]]
Before you start any calculations we can decide how many '''G'''-vectors you want use to represent your wave-function. By default Yambo will use all of them, and for the present tutorial this is fine, however if you are studying larger systems you would like to reduce them in order to speed-up calculations, you can do it with <code> yambo -i -V RL</code> and then changing the variable <code>MaxGvecs</code> that referees to Ng in the previous formula. 

Now we will proceed in the calculation of the [http://en.wikipedia.org/wiki/Hartree%E2%80%93Fock_method Hartree-Fock(HF)] exchange. This is composed of two terms, that Hartree and the Fock (or exchange) one:

[[File:hf.png|Hartree Fock]]
In this tutorial we will calculate only the first order correction to the Kohn-Sham Hamiltonian due to the exchange term. Because of we are working in periodic system, the most appropriate basis to represent the Coulomb potential, appearing in the Fock term, is a plane-wave basis:

[[File:v_q_plus_G.png|Coulomb potential in plane wave]]
In order to generate the input file for the exchange type <code>yambo -x</code>. The variable that governs the number of '''G''' vectors Nex in the Coulomb potential is <code>EXXRLvcs</code>. In addition notice that in the previous formula for V('''r'''-'''r'''') we have an integral on the '''q''' vector, that in the code is discretized on a regular '''q'''-grid generated from the '''k'''-point one, '''q'''='''k'''-'''k''''.

==== K-points convergence ====

Enter the YAMBO folder

<code> >cd YAMBO/ >ls Convergence_Plots 2x2x2 4x4x4 6x6x6 8x8x8 Gamma</code> 

Enter each grid folder and run <code>>yambo</code> without options. Then type

 
<code> >yambo -x -F INPUTS/01HF_corrections</code>
and edit the 01HF_corrections file

<code> HF_and_locXC # [R XX] Hartree-Fock Self-energy and Vxc EXXRLvcs= 7 Ry # [XX] Exchange RL components %QPkrange # [GW] QP generalized Kpoint/Band indices 1| 8| 1| 15| % %QPerange # [GW] QP generalized Kpoint/Energy indices 1| 8| 0.0|-1.0| %</code>
setting

<code> EXXRLvcs=7 Ry</code>
Then run in each k-point folder

<code> >yambo -F INPUTS/01HF_corrections -J HF_7Ry</code>
Note that after the each run Yambo produces three output file, one starting with <code>r_...</code> , another with <code>l_...</code> and a third one starting with <code>o_...</code>. The first one is a ''report'' of the actual calculation with all the details of the system, input, and results, while the second is a ''log'' with the running time of each process.

The file we are most interested in is the output file, <code>o-HF_7Ry.hf</code>. This file contains several columns. The fourth, labelled with <code>Ehf</code> represents the Hartree-Fock energy. This is the quantitu we have to look at.

==== G-vectors convergence ====

Enter the <code>4x4x4</code> folder and edit the <code>01HF_corrections</code> file changing the field <code>EXXRLvcs=</code>3,6,7 and 15 Ry. For each case run

<code> >yambo -F INPUTS/01HF_corrections -J HF_???Ry</code>
with <code>???</code>=3,6,7 and 15

The results of this series of calculations are summarized in the following plots. Note the rapid convergence with the number of k-points.

To obtain the plots of the following graphs just plot the columns <code>#4-#3</code> versus <code>#3</code> of the <code>o.hf</code> files.

{|
| [[File:HF_parameters.png|Convergence Hartree-Fock calculations]]
| [[File:HF_gap.png|Convergence Hartree-Fock gap silicon]]
|}

=== COHSEX without empty bands ===

The Hartree-Fock self-energy just described in the previous section, although successful on some molecular systems, miserably fails in extended systems. The reason of this failure lies in the fact that electrons can screen the Coulomb potential, and therefore one electron feels a screened potential instead of the bare one. A common approximation for this screened potential is the so-called Random Phase Approximation:

[[File:gw.png|Hartree Fock]]
 

where the bare Coulomb potential V('''r''') is replaced by a non-local and frequency dependent one W('''r''','''r'''',ω). Subsequently it is possible to redefine all the perturbation theory in term of this screened potential, and disregarding the additional corrections coming from the vertex part, one obtains the so-called [http://localhost/yambo_web_page/theory/lectures.php#GW GW] approximation.

However the substantial complexity associated with calculating the non-local, energy dependent Σ=GW operator inspired early efforts to find simplifying approximations as the static COHSEX approximation prosed by Hedin[[[#hedin|4]]]. The Coulomb Hole plus Screened Exchange (COHSEX) approximation[[[#march|2]],[[#fardi|3]]] eliminates the summation over empty states for the self energy operator and has the added benefit of being a static operator, a particular simplification for self consistent calculations. With the COHSEX approximation the self-energy is composed of two parts:

[[File:gw_sex.png|Screened Exchange]]
[[File:gw_coh.png|Cuolomb Hole]]
 

where Wp=W - V. 
In order to calculate the COHSEX self-energy with yambo you need first the static screened interaction <code>yambo -b -k hartree</code>. As for the V('''r''') case, also W('''r''','''r'''',E=0) will depend from the number of '''G'''-vectors, and the '''k'''-grid, but this time also the number of conduction bands <code>XsBndsRn</code> will enter in the screening calculation through the polarization function, see [http://www.yambo-code.org/theory/docs/doc_Xd.php The Interacting response function: Many-Body and TDDFT] section. Notice however that there are not any additional dependence of the self-energy operator from the conduction bands. After you obtained the screened interaction you are ready to build the self-energy operator and solve the corresponding Dyson equation, have a look to the [http://www.yambo-code.org/theory/docs/doc_GW.php Dyson Equation solvers] in Yambo. In order to get the quasi-particle energies, just do <code>yambo -b -g n -k hartree</code>. After calculation are completed Yambo will produce an output file <code>o.qp</code> which contains the values of the bare and re-normalized energy levels.

==== K-points convergence ====

Follow the same strategy of the HF case. Enter each k-point folder and type

<code> > yambo -b -k hartree -g n -p c -F INPUTS/02Cohsex</code>
edit the input file and change the values of the fields

<code> EXXRLvcs=7 Ry %BndsRnXs 1 | 10 | # [Xs] Polarization function bands % NGsBlkXs= 1 RL # [Xs] Response block size #UseEbands # [GW] Force COHSEX to use empty bands %QPkrange # [GW] QP generalized Kpoint/Band indices 1| 8| 1| 10| %</code>
leaving the other parameters unchanged. Now, in each k-point folder, run

<code> >yambo -F INPUTS/02Cohsex -J Cohsex_HF7Ry_X0Ry-nb10</code>
==== W size convergence ====

Enter the <code>4x4x4</code> folder and edit the <code>02Cohsex_corrections</code> file changing the field <code>NGsBlkXs=</code>3,6,7 Ry. Run

<code> >yambo -F INPUTS/02Cohsex -J Cohsex_HF7Ry_X???Ry-nb10 </code>
with <code>???</code>=3,6,7 and 15

==== W bands ====

Open your input file and change only the input variable <code>NGsBlkXs=1 Ry. Then change</code> <code> %BndsRnXs 1 | 20 | # [Xs] Polarization function bands %</code>

and run <code>yambo -F INPUTS/02Cohsex -J Cohsex_HF7Ry_X1Ry-nb20</code>. Repeat the calculations using 30 and 40 bands changing <code>nb???</code> in the job string identifier. Finally check how the Chosex Direct and Indirect band gap behave as a function of the number of bands in the screening.

==== COHSEX with empty bands ====

While the Screened Exchange(SEX) part of the COHSEX self-energy has a structure similar to the Hartree-Fock exchange term, the Coulomb Hole(COH) acts as static external potential on the electrons. In the COH part the delta function δ('''r'''-'''r'''') comes from the completeness relation:

[[File:completeness.png|Completeness relation]]
Now we avoid the use of this relation in such a way to have a self-energy that depends from the conduction bands too. This can be done uncommenting flags <code>UseEbands</code> and setting the number of bands in the Green's function: <code> % GbndRnge 1 | 10 | # [GW] G[W] bands range %</code> Repeat the previous calculations with different <code>GbndRnge</code> for instance, 10 20 30 40, and check how the COHSEX direct and indirect band gap behave as a function of the number of bands in the Green's function. 
Recently an enhanced version of the COHSEX approximation has been proposed, if you want learn more have a look to the reference[[[#hybertsen|4]]].

[[File:Cohsex_gap.png|COHSEX convergence]]
=== The plasmon pole approximation ===

Even the static COHSEX approximation is very appealing, it was clear from the first calculation that dynamical effects cannot be disregarded in solids[[[#strinati|6]]]. This fact motivated the research for approximated way to deal with a frequency dependent interaction, and one of the first proposal was the so-called [[../../theory/docs/doc_Xp.php|Plasmon-Pole Approximation (PPA)]] (see ref. [[[#godby|7]]]).

Now we will proceed to the calculation of the silicon band gap in G0W0 within PPA. In each section you will be asked to perform several calculations varying the value of the relevant variables involved. More specifically let's consider a typical Yambo input file to calculate GW corrections in the PPA.

<code> gw0 # [R GW] GoWo Quasiparticle energy levels ppa # [R Xp] Plasmon Pole Approximation HF_and_locXC # [R XX] Hartree-Fock Self-energy and Vxc em1d # [R Xd] Dynamical Inverse Dielectric Matrix EXXRLvcs= 7 Ry # [XX] Exchange RL components % QpntsRXp 1 | 8 | # [Xp] Transferred momenta % % BndsRnXp 1 | 30 | # [Xp] Polarization function bands % NGsBlkXp= 7 Ry # [Xp] Response block size % LongDrXp 1.000000 | 0.000000 | 0.000000 | # [Xp] [cc] Electric Field % PPAPntXp= 27.21138 eV # [Xp] PPA imaginary energy % GbndRnge 1 | 30 | # [GW] G[W] bands range % GDamping= 0.10000 eV # [GW] G[W] damping dScStep= 0.10000 eV # [GW] Energy step to evalute Z factors DysSolver= "n" # [GW] Dyson Equation solver (`n`,`s`,`g`) %QPkrange # [GW] QP generalized Kpoint/Band indices 1| 8| 1| 10| % %QPerange # [GW] QP generalized Kpoint/Energy indices 1| 8| 0.0|-1.0| %</code>
The variables are the same of the COHSEX case plus a new one <code>PPAPntXp</code> that describes the imaginary energy used to fit the Plasmon Pole model. 
Follow the same strategy of the COHSEX case. Enter each k-point folder and type:

 
<code> yambo -d -k hartree -g n -p p -F INPUTS/03GoWo_PPA_corrections</code> 

otherwise you can use the existent file <code>Input/03GoWo_PPA_corrections</code>. Now you have to study the convergence of the G0W0 gap versus the number of k-points, the number of bands in χ <code>BndsRnXs</code>, the size of the dielectric constant <code>NGsBlkXs</code> and the number of bands in the Green's function <code>GbndRnge</code>.

Please follow the same strategy of the COHSEX case running yambo using

<code> yambo -F INPUTS/03GoWo_PPA_corrections -J GoWo_PPA_HF7Ry_X???Ry-nb???_nb???</code>
The final convergence plots should look like these.

{|
| [[File:GoWo_PPA_parameters.png|G0W0 Convergence]]
| [[File:GoWo_PPA_gap.png|G0W0 silicon gap]]
|}

 

Final runs!! Now you know how to converge a G0W0 calculation so you can decide which are the parameters needed for full convergence. First do a COHSEX and then a GoWo (PPA) run at convergence, and you should obtain results similar to the following graph:

[[File:Si_gap.png|Final Gap Silicon]]
 

Curiosity: What's happen if the PPA fails? Have a look to the tutorial on the [http://www.yambo-code.org/tutorials/Real_Axis_and_Lifetimes/index.php Real-Axis Integration].

== References ==

# [http://en.wikipedia.org/wiki/Silicon Silicon on wikipedia].
# [http://www.amazon.com/Electron-Correlation-Solid-State-Norman/dp/1860942008 Electron Correlation in the Solid State], Norman H. March (1999).
# [http://prb.aps.org/abstract/PRB/v38/i11/p7530_1 GW approach to the calculation of electron self-energies in semiconductors], B. Farid et al., Phys. Rev. B '''38''', 7530 (1988).
# [http://prola.aps.org/abstract/PR/v139/i3A/pA796_1 New Method for Calculating the One-Particle Green's Function with Application to the Electron-Gas Problem] L. Hedin, Phys. Rev. '''139''', A796 (1965).
# [http://arxiv.org/abs/1008.4320 Enhanced Static Approximation to the Electron Self-Energy Operator for Efficient Calculation of Quasiparticle Energies], Wei Kang, Mark S. Hybertsen, Phys. Rev. B '''82''', 195108 (2010).
# [http://prl.aps.org/abstract/PRL/v45/i4/p290_1 Dynamical Correlation Effects on the Quasiparticle Bloch States of a Covalent Crystal], G. Strinati, H. J. Mattausch, and W. Hanke , Phys. Rev. Lett. '''45''', 290 (1980).
# [http://www-users.york.ac.uk/~rwg3/Papers/Paper_34.pdf Space-time method for ab initio calculations of self-energies and dielectric response functions of solids], H. N. Rojas, R. W. Godby, and R. J. Needs, Phys. Rev. Lett. '''74''', 1827 (1995) .

GW - Revision history

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Yambowikiadmin: Created page with "=== Basic concepts of the GW approximation by the Yambo Team === G0W0 In this tutorial you will learn the basic concepts of the [http://www.yambo-co..."

Yambowikiadmin: Created page with "=== Basic concepts of the GW approximation
by the Yambo Team === G0W0 In this tutorial you will learn the basic concepts of the [http://www.yambo-co..."