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5-dimensional Kerr-AdS spacetime with a Nambu-Goto string --- generic case with global AdS coordinates
License: GPL3
Image: ubuntu2004
5D Kerr-AdS spacetime with a Nambu-Goto string
Generic case (a,b) in global AdS coordinates
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 :
In this notebook, we set
Possible particular cases:
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 :
Conformal metric at the boundary (check of Eq. (2.11))
The conformal metric:
Let us introduce a function to perform asymptotic expansions up to a given order:
Expansion to order provides the conformal metric on the boundary :
This agrees with Eq. (2.11); in particular, we have
Global AdS coordinates
The transition from the Boyer-Lindquist coordinates to the global AdS coordinates is derived from Eq. (5.24) of S.W. Hawking, C.J. Hunter & M.M. Taylor-Robinson, Phys. Rev. D 59, 064005 (1999):
The following assumptions are required to perform simplifications:
We import the function simplify_sqrt_real
to simplify some square roots, which would not be simplified with simplify_full
:
Check:
Remark: despite the rather complicated relation between and , the ratio depends only on and takes a simple form: Indeed:
Metric components in global ADS coordinates
For generic values of , Sage does not succeed in computing the components of the metric tensor in a reasonable time. Only for or it manages to do so. For , the expression is cumbersome, but for , one gets a rather simple expression:
Asymptotic form of the metric in ADS coordinates (check of Eq. (2.17))
For , the metric tensor can be approximated by , the expression of the latter in ADS coordinates being given by Eq. (3.27) of Gibbons, Perry & Pope, CQG 22, 1503 (2005) (arXiv:hep-th/0408217) (our Eq. (2.17)):
In the above expression, we do not have specified . Its explicit expression in terms of , and is
Check of Eq. (2.17) for :
For , and differ only by a term proportional to :
This difference is only of order :
Setting the metric to its asymptotic form:
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. (4.27) of the paper):
Induced metric on the string worldsheet
The string worldsheet metric is the metric induced by the spacetime metric , i.e. the pullback of by the embedding :
Because of the bug #27492, which impedes parallel computations involving symbolic functions, such as , we set back to serial computations:
Nambu-Goto action
The determinant of is
Let us define a function for expansions in and up to a given order:
Expanding at fourth order in and (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 and :
Euler-Lagrange equations
We compute the Euler-Lagrange equations from for and :
Solving the equation for (Eq. (4.29))
We recover Eqs. (4.29) with and .
The symbolic constants and are actually denoted _K1
and _K2
by SageMath, as print
reveals:
Hence we perform the substitutions with SR.var('_K1')
and SR.var('_K2')
:
Solving the equation for (Eq. (4.29))
We recover Eq. (4.29) with and .
Nambu-Goto Lagrangian at fourth order in and
The equation for
We plug the solutions obtained previously for and in this equation:
Check of Eq. (4.30)
The equation for is thus:
Given that and we get for the following equation for (defining ):
This agrees with Eq. (4.30) of the paper.
Solving the equation for
The solution involves an integral that SageMath is not capable to evaluate with the default integrator. Printing Y_sol
provides 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(y)
represents the integral , whose integrand, say, is read from the output of print(Y_sol(Y))
:
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. (4.31) (expression of )
The term involving the constant agrees with that of Eq. (4.31):
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. (4.31), once we express in terms of :
The denominator agrees with Eq. (4.31) as well:
Let us remove the arctan term from :
The coefficient of the log term is
The numerator and denominator both agree with Eq. (4.31):
Given that we have
Hence the term in agrees with the corresponding term in Eq. (4.30).
Finally, the last term in is
This term agrees with Eq. (4.31), given the simplification .
Conjugate momenta
:
:
Check of Eq. (4.33)
We start from as given by Eq. (4.32):
Let us perform an expansion in for :
We consider :
The term in factor of is
Hence this terms agrees with Eq. (4.32). 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. (4.33).
We remove it:
The coefficient of the term in is
This is in agreement with Eq. (4.33).
Finally the remaining term is
The denominator clearly agrees with Eq. (4.33).
Conclusion: we have full agreement with Eq. (4.33).