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5-dimensional Kerr-AdS spacetime with a Nambu-Goto string
License: GPL3
Image: ubuntu2004
5D Kerr-AdS spacetime with a Nambu-Goto string
Case b = n a
This SageMath notebook is relative to the article Heavy quarks in rotating plasma via holography by Anastasia A. Golubtsova, Eric Gourgoulhon and Marina K. Usova, arXiv:2107.11672.
The involved differential geometry computations are based on tools developed through the SageManifolds project.
NB: a version of SageMath at least equal to 9.1 is required to run this notebook:
First we set up the notebook to display mathematical objects using LaTeX rendering:
Since some computations are quite long, we ask for running them in parallel on 8 cores:
Spacetime manifold
We declare the Kerr-AdS spacetime as a 5-dimensional Lorentzian manifold:
Let us define Boyer-Lindquist-type coordinates (rational polynomial version) on , via the method chart()
, the argument of which is a string expressing the coordinates names, their ranges (the default is ) and their LaTeX symbols:
The coordinate is related to the standard Boyer-Lindquist coordinate by
The coordinate ranges are
Note that contrary to the 4-dimensional case, the range of is only (cf. Sec. 1.2 of R.C. Myers, arXiv:1111.1903 or Sec. 2 of G.W. Gibbons, H. Lüb, Don N. Page, C.N. Pope, J. Geom. Phys. 53, 49 (2005)). In other words, the range of is only.
Metric tensor
The 4 parameters , , and of the Kerr-AdS spacetime are declared as symbolic variables, and being the two angular momentum parameters and being related to the cosmological constant by :
We assume that :
Some auxiliary functions:
The metric is set by its components in the coordinate frame associated with the Boyer-Lindquist-type coordinates, which is the current manifold's default frame. These components can be deduced from Eq. (5.22) of the article S.W. Hawking, C.J. Hunter & M.M. Taylor-Robinson, Phys. Rev. D 59, 064005 (1999) (the check of agreement with this equation is performed below):
Check of Eq. (2.9)
We need the 1-forms , , , and :
In agreement with , we introduce the 1-form with since :
Check of Eq. (2.9):
Einstein equation
The Ricci tensor of is
Let us check that is a solution of the vacuum Einstein equation with the cosmological constant :
String worldsheet
The string worldsheet as a 2-dimensional Lorentzian submanifold of :
Let us assume that the string worldsheet is parametrized by :
The string embedding in Kerr-AdS spacetime, as an expansion about a straight string solution in AdS (Eq. (4.5) of the paper):
Induced metric on the string worldsheet
Because of the bug #27492, which impedes parallel computations involving symbolic functions, such as , we switch back to serial computations:
The metric on the string worldsheet is the metric induced by the spacetime metric , i.e. the pullback of by the embedding :
Nambu-Goto action
The determinant of is
Expanding at fourth order in (will be required latter):
For the time being, only the expansion at second order in is required:
The Nambu-Goto Lagrangian at second order in :
Euler-Lagrange equations
We compute the Euler-Lagrange equations at order for and :
Solving the equation for (Eq. (4.8))
We recover Eqs. (4.8) with and .
The symbolic constants and are actually denoted _K1
and _K2
by SageMath, as the print
reveals:
Hence we perform the substitutions with SR.var('_K1')
and SR.var('_K2')
:
Solving the equation for (Eq. (4.8))
We recover Eq. (4.8) with and .
Nambu-Goto Lagrangian at fourth order in
The equation for
We plug the solutions obtained previously for and in this equation:
Check of Eq. (4.9)
The equation for is thus:
Let us define
Given that and we get the equation for :
This agrees with Eq. (4.9) of the paper.
Solving the equation for
We use the function desolve
to solve the differential equation for :
The solution involves an integral that SageMath is not capable to evaluate with the default integrator. Trying to display Y_sol
would make SageMath hang. Instead, we print Y_sol
to get the unvaluated form of the integral, in order to compute it by means of FriCAS:
The solution involves some constant, denoted _C
by SageMath. We rename it C_1
and rewrite the above solution as
Integ(r)
represents the integral , whose integrand, say, is read from the output of print(Y_sol(r))
:
We split the integral in two parts: with and
Check:
Let us evaluate by means of FriCAS:
Check:
Similarly, we evaluate by means of FriCAS:
Check:
In the above expressions for and there appears , which can be rewritten where is the positive root of . More precisely, we perform the following substitution:
In the second , we recognize the function, via the identity Given that , we use this identity as
Thus, we perform the following substitution, disregarding the additive constant :
Let us check that we have indeed a primitive of :
Similarly, let us express in terms of :
Again, we use the identity to rewrite as
Let us also replace by in order to have the same log term as in :
Let us check that we have indeed a primitive of :
The full integral is thus
so that the solution is
Let us check that Y_sol
is indeed a solution of the differential equation for :
Check of Eq. (4.10) (expression of )
The term involving the constant agrees with that of Eq. (4.10):
Let us remove it from and divide the result by :
The coefficient of the arctan term is
The numerator of this term agrees with Eq. (4.10):
The denominator agrees with Eq. (4.10) as well:
Let us remove the arctan term from :
The coefficient of the log term is
Check against Eq. (4.10):
Given that we have
Hence the term in agrees with the corresponding term in Eq. (4.10).
Finally, the last term in is
This term agrees with Eq. (4.10), given the simplification .
Conclusion: we have full agreement with Eq. (4.10).
Conjugate momenta
Check of Eq. (4.15):
Check of Eq. (4.14):
We start from as given by Eq. (4.13):
Let us perform an expansion in for :
We consider :
The term in factor of is
It is a constant term, of the type , in agreement with Eq. (4.14). We remove it from the main term:
Let divide both the numerator and denominator by :
The coefficient of the term in is
This is in agreement with Eq. (4.14).
We remove it:
The coefficient of the term in is
This is in agreement with Eq. (4.14).
Finally the remaining term is
The denominator clearly agrees with Eq. (4.14); the numerator agrees as well:
Conclusion: we have full agreement with Eq. (4.14).