Module-3 Ab Initio Molecular Dynamics April 01 & April 06
Feb 01, 2016
Module-3
Ab Initio Molecular Dynamics
April 01 & April 06
Ab Initio MD: Born-Oppenheimer MD
HBOMD({RI}, {PI}) =NX
I=1
P2I
2MI+ Etot({RI})
=NX
I=1
P2I
2MI+
min{ }
nD
({ri}, {RI})�
�
�
Hel
�
�
�
({ri}, {RI})Eo
+NX
J>I
ZIZJ
RIJ
rRI
D |Hel| |
E=DrRI |Hel| |
E+D |rRI Hel| |
E+D |Hel|rRI |
E
6=D |rRI Hel| |
E
Basis set should be large enough! Convergence of wave function and energy conservation:
Time step (fs)
Convergence (a.u.)
conservation (a.u./ps)
CPU time (s) for 1 ps
trajectory
0.25 10-6 10-6 16590
1 10-6 10-6 4130
2 10-6 6 x 10-6 2250
2 10-4 1 x 10-3 1060
Concerns:Wavefunction optimisation at every MD step is time consuming!
Note: wfn has to be well converged.
Car-Parrinello MD
Basic Idea:
Timescale separation: Electronic part is fastNuclear part is slow
Classical mechanical adiabatic energy-scale separation
making 2 classical subsystems that are adiabatically energy-
scale separated.
1. nuclear coordinates2. orbital coefficients
Lagrangian: LCP =
X
I
1
2
MI˙R2I +
X
i
µi
D˙ i| ˙ i
E
�D 0
��� ˆHel
��� 0
E+ constraints
is the molecular orbital (spatial)
0 is the Slater det.
µ is the fictitious mass for orbitals
i =X
⌫
c⌫i�⌫
Note: LCP ⌘ LCP(RN , RN , n, n)
d
dt
@L@RI
=@L@RI
Equations of motion can be computed as
LCP ⌘ LCP(RN , RN , n, n)
d
dt
�L�D i
���=
�L� h i|
µi¨ i = � �
� h i|D 0
��� ˆHel
��� 0
E+
�
� h i| (constraints)
FI = � @
@RI
D 0
��� ˆHel
��� 0
E+
@
@RI(constraints)
Within the KS theory constraints are due to orthonormality of orbitals:X
i
X
j
⇤ij (h�i|�ji � �ij)
Nuclear temperature(physical temperature): T /
X
I
MIR2I
Fictitious temperature: T orb. /X
i
µi
D�i|�i
E
No energy transfer between physical system and the orbital (quasi-adiabatic separation of dynamics)
Orbitals should move close to the corresponding Born-Oppenheimer solutions: Torb has to be small enough
(close to zero K ⇒“cold electrons”)
Energy transfer from “hot nuclei” to “cold electrons” should be strictly avoided during the dynamics
No overlap in the vibrational density of states(orbital motion has to be much above 4000 cm-1)
Thus motion can be kept adiabatically separable!
Energy is well conserved (no noise due to
SCF procedure!)
Thus, motion about the actual BO surfaceHigh freq. oscillations are not relevant in the timescale of the nuclear dynamics: thus not
only averages, but also time-dependent properties can also be computed
Time step should be small (to sample high freq. motion of orbital degrees of freedom):
usually about 0.06-0.12 fs
(Very small) Fictitious mass should be appropriately chosen (400-700 au)
Energy conservation can be checked to verify the accuracy of dynamics.
CP/5 a.u. /—
CP/10 a.u. /—
BO/10 a.u. /10-6
BO/100 a.u. /10-6
BO/100 a.u. /10-5
BO/100 a.u. /10-4
• Computationally efficient• Better energy conserving
• Not truly an BO MD; dynamics could get affected if parameters are not chosen
properly.• Small tilmestep (~1/10 smaller)
• Adiabatic separation doesn’t work in some cases (zero band gap)
• Better wfn extrapolation algorithms are available today; thus wfns can be
converged fast, and BOMD can be made computationally efficient!