Abstract
In this article, we propose high-order finite difference schemes for the equations of relativistic hydrodynamics, which are entropy stable. The crucial components of these schemes are a computationally efficient entropy conservative flux and suitable high-order entropy dissipative operators. We first design a higher-order entropy conservative flux. For the construction of appropriate entropy dissipative operators, we derive entropy scaled right eigenvectors. This is then used with ENO-based sign-preserving reconstruction of scaled entropy variables, which results in higher-order entropy-stable schemes. Several numerical results are presented up to fourth order to demonstrate entropy stability and performance of these schemes.
Similar content being viewed by others
References
Abramowitz, M., Stegun, I.A.: Handbook of Mathematical Functions: With Formulas, Graphs, and Mathematical Tables. Dovers Publications, Inc., New York (1972)
Aloy, M.A., Ibáñez, J.M., Martí, J.M., Müller, E.: GENESIS: a high-resolution code for three-dimensional relativistic hydrodynamics. Astrophys. J. Suppl. Ser. 122(1), 151–166 (1999)
Anile, A.M.: Relativistic Fluids and Magneto-Fluids: With Applications in Astrophysics and Plasma Physics. Cambridge University Press, Cambridge (1989)
Barth, T.J.: Numerical methods for gas-dynamics systems on unstructured meshes. In: Kroner, D., Ohlberger, M., Rohde, C. (eds.) An Introduction to Recent Developments in Theory and Numerics of Conservation Laws. Lecture Notes in Computational Science, vol. 5, pp. 195–285. Springer, Berlin (1999)
Begelman, M.C., Blandford, R.D., Rees, M.J.: Theory of extragalactic radio sources. Rev. Mod. Phys. 56(2), 255–351 (1984)
Boettcher, M., Harris, D.E., Krawczynski, H.: Relativistic Jets from Active Galactic Nuclei. Wiley, Hoboken (2012)
Centrella, J., Wilson, J.R.: Planar numerical cosmology. II. The difference equations and numerical tests. Astrophys. J. Suppl. Ser. 54(2), 229–249 (1984)
Chandrashekar, P.: Kinetic energy preserving and entropy stable finite volume schemes for compressible Euler and Navier–Stokes equations. Commun. Comput. Phys. 14(5), 1252–1286 (2013)
Chiodaroli, E., Lellis, C.D., Kreml, O.: Global Ill-posedness of the isentropic system of gas dynamics. Commun. Pure Appl. Math. 68(7), 1157–1190 (2015)
Choi, E., Ryu, D.: Numerical relativistic hydrodynamics based on the total variation diminishing scheme. New Astron. 11(2), 116–129 (2005)
Falle, S.A.E.G., Komissarov, S.S.: An upwind numerical scheme for relativistic hydrodynamics with a general equation of state. Mon. Not. R. Astron. Soc. 278(2), 586–602 (1996)
Fjordholm, U.S., Mishra, S., Tadmor, E.: Arbitrarily high-order accurate entropy stable essentially nonoscillatory schemes for systems of conservation laws. SIAM J. Numer. Anal. 50(2), 544–573 (2012)
Fjordholm, U.S., Mishra, S., Tadmor, E.: ENO reconstruction and ENO interpolation are stable. Found. Comput. Math. 13(2), 139–159 (2013)
Font, J.A.: Numerical hydrodynamics and magnetohydrodynamics in general relativity. Living Rev. Relativ. 11(1), 7 (2008)
Godlewski, E., Raviart, P.-A.: Hyperbolic Systems of Conservation Laws. Ellipses, Paris (1991)
Gottlieb, S., Shu, C.-W., Tadmor, E.: Strong stability-preserving high-order time discretization methods. SIAM Rev. 43(1), 89–112 (2001)
Harten, A.: High resolution schemes for hyperbolic conservation laws. J. Comput. Phys. 49(3), 357–393 (1983)
Ismail, F., Roe, P.L.: Affordable, entropy-consistent euler flux functions II: entropy production at shocks. J. Comput. Phys. 228(15), 5410–5436 (2009)
Jiang, G.-S., Shu, C.-W.: Efficient implementation of weighted ENO schemes. J. Comput. Phys. 126(1), 202–228 (1996)
Landau, L.D., Lifschitz, E.M.: Fluid Mechanics. CHapter XV - Relativistic Fluid Dynamics, 2nd edn. Pergamon, New York (1987)
LeFloch, P.G., Mercier, J.M., Rohde, C.: Fully discrete entropy conservative schemes of arbitrary order. SIAM J. Numer. Anal. 40(5), 1968–1992 (2002)
Martí, J.M., Müller, E.: Extension of the piecewise parabolic method to one-dimensional relativistic hydrodynamics. J. Comput. Phys. 123(1), 1–14 (1996)
Martí, M.J., Müller, E.: Grid-based methods in relativistic hydrodynamics and magnetohydrodynamics. Living Rev. Comput. Astrophy. 1(1), 3 (2015)
Martí, M.J., Müller, E.: Numerical hydrodynamics in special relativity. Living Rev. Relativ. 6(1), 7 (2003)
Mignone, A., Bodo, G.: An HLLC Riemann solver for relativistic flows I. Hydrodynamics. Mon. Not. R. Astron. Soc. 364(1), 126–136 (2005)
Mignone, A., Plewa, T., Bodo, G.: The piecewise parabolic method for multidimensional relativistic fluid dynamics. Astrophys. J. Suppl. Ser. 160(1), 199–219 (2005)
Mirabel, I.F., Rodríguez, L.F.: Sources of relativistic jets in the galaxy. Ann. Rev. Astron. Astrophys. 37, 409–443 (1999)
Rosa, J.N.D.L., Munz, C.-D.: XTROEM-FV: a new code for computational astrophysics based on very high order finite-volume methods-II. Relativistic hydro- and magnetohydrodynamics. Mon. Not. R. Astron. Soc. 460(1), 535–559 (2016)
Ryu, D., Chattopadhyay, I., Choi, E.: Equation of state in numerical relativistic hydrodynamics. Astrophys. J. Suppl. Ser. 166(1), 410–420 (2006)
Schneider, V., Katscher, U., Rischke, D.H., Waldhauser, B., Maruhn, J.A., Munz, C.-D.: New algorithms for ultra-relativistic numerical hydrodynamics. J. Comput. Phys. 105(1), 92–107 (1993)
Sen, C., Kumar, H.: Entropy stable schemes for ten-moment Gaussian closure equations. J. Sci. Comput. 75(2), 1128–1155 (2018)
Sweby, P.K.: High-resolution schemes using flux limiters for hyperbolic conservation laws. SIAM J. Numer. Anal. 21(5), 995–1011 (1984)
Synge, J.L.: Relativity: The Special Theory. North-Holland Pub. Co., Amsterdam (1956)
Tadmor, E.: The numerical viscosity of entropy stable schemes for systems of conservation laws. I. Math. Comput. 49(179), 91–103 (1987)
Wilson, J.R.: A numerical method for relativistic hydrodynamics. In: Smarr, L.L. (ed.) Sources of Gravitational Radiation. Proceedings of the Battelle Seattle Workshop, July 24–August 4, 1978, pp. 423–445. Cambridge University Press, Cambridge (1979)
Wu, K., Tang, H.Z.: High-order accurate physical-constraints-preserving finite difference WENO schemes for special relativistic hydrodynamics. J. Comput. Phys. 298, 539–564 (2015)
Wu, K., Tang, H.Z.: Physical-constraints-preserving central discontinuous Galerkin methods for special relativistic hydrodynamics with a general equation of state. Astrophys. J. Suppl. Ser. 228(3), 23 (2016)
Zanna, L.D., Bucciantini, N.: An efficient shock-capturing central-type scheme for multidimensional relativistic flows I. Hydrodynamics. Ann. Rev. Astron. Astrophys. 390(3), 1177–1186 (2002)
Zensus, J.A.: Parsec-scale jets in extragalactic radio sources. Ann. Rev. Astron. Astrophys. 35(1), 607–636 (1997)
Zhang, W., MacFadyen, A.I.: RAM: a relativistic adaptive mesh refinement hydrodynamics code. Astrophys. J. Suppl. Ser. 164(1), 255–279 (2006)
Acknowledgements
We want to thank Prof. Praveen Chandrashekar (TIFR-CAM, Bengaluru, India) and Prof. Dinshaw Balsara (Notre-Dame University, IN, USA) for several useful discussions. We also want to thank Prof. José María Martí (Universidad de Valencia, Spain) for providing us the codes for the exact solutions of the Riemann problems.
Author information
Authors and Affiliations
Corresponding author
Additional information
Publisher's Note
Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
Appendices
Computation of primitive variables
The RHD equations involve the conserved quantities, D, \(\varvec{m}\) and E; but to solve the RHD equations numerically, we need to know the explicit values of the primitive variables, \(\rho \), \(\mathbf{u}\) and p. The primitive variables can be extracted by inverting the RHD equations (1). For the ideal equation of state (4), [30] showed that (using Eq. (1)) the variable \({u} (=|\mathbf{u}|)\) satisfies
where
with \(M=(m_x^2+m_y^2+m_z^2)^{1/2}\). Equation (25) could either be solved using the analytical methods or using an approximate root solver. In [30], authors have suggested the following expressions for the lower bound \(u_{\mathrm{lb}}\) and upper bound \(u_{\mathrm{ub}}\):
and
where \(\delta \approx 10^{-6}\). Furthermore, to find the root of Eq. (25) using the Newton–Raphson method, [30] suggested the initial guess \(u_o\) as,
where \(z=\frac{1}{2}\left( 1-\frac{D}{E}\right) (u_{\mathrm{lb}}-u_{\mathrm{ub}})\) if \(u_{\mathrm{lb}}>10^{-9}\) and \(z=0\) otherwise. We then obtain \(u_o\) between \(u_{\mathrm{lb}}\) and \(u_{\mathrm{ub}}\). Also, an accuracy of nine digits can be achieved in at most five iterations of the Newton–Raphson root solver.
For the analytic solution, we can use the direct formulation of the roots of the quartic equations. The general form of analytical roots is available in [1]. We note that Eq. (25) has two complex roots and two real roots. Among two real roots, only one root lies between the lower and upper bounds suggested by [30], which is given by,
where,
Once we have the value of u, we can find all the primitive variables, i.e. \(\rho ,\ u_i, \ p,\) using the expressions
In this article, we use numerical approach to find the primitive variables from the conservative variables.
Entropy scaled right eigenvectors
In this section, we present the entropy scaled right eigenvectors. First, we consider the case of x-direction right eigenvectors. We rewrite the RHD system (3),
Following [29], the eigenvalues of the Jacobian matrix \(\mathbf {A}^x\) are given by:
Here, \(Q^x=1-u_x^2-c^2 u_y^2\) and c is the sound speed given by the expression
where \(n=k-1\) with \(k = \frac{\gamma }{\gamma -1}\), for all \(\mathbf {U} \in \Omega \). Note that \(Q^x=1-u_x^2-c^2 u_y^2 > 0\); therefore, all the eigenvalues are real. A straightforward calculation results in the following expressions for the eigenvectors in primitive variables:
The eigenvector matrix for the conservative system, \(\tilde{\mathbf {R}}^x\), can be derived using,
where \(\tilde{\mathbf {R}}_w^{x} =(e_1, \ e_2, \ e_3,\ e_4)\), i.e. the matrix of right eigenvectors for the primitive system. To obtain the scaled right eigenvector matrix \({{\mathbf {R}}}^x\), we need to find a scaling matrix \(\mathbf {T}^x\) such that the scaled right eigenvector matrix, \({{\mathbf {R}}}^x= \tilde{\mathbf {R}}^x \mathbf {T}^x\), satisfies
We first derive the expression of the entropy scaled right eigenvector for the primitive variable system, \({\mathbf {R}}^x_w\). Following the procedure of [4, 31], the scaling matrix \(\mathbf {T}^x\) is the square root of the matrix \(\mathbf {Y}^x\), where
which on a long calculation results in,
Consequently,
So, the entropy scaled right eigenvector matrix for the primitive system is given by
where
Using Eq. (26), we can calculate the entropy scaled right eigenvectors for the conservative system satisfying (27).
Remark B.1
Proceeding similarly in the y-direction, we get the eigenvalues of the Jacobian matrix as
and the right eigenvector matrix, for the system in primitive variables, as
where \(Q^y=1-u_y^2-c^2 u_x^2\). Consequently, the entropy scaled right eigenvector matrix is given by
where
Rights and permissions
About this article
Cite this article
Bhoriya, D., Kumar, H. Entropy-stable schemes for relativistic hydrodynamics equations. Z. Angew. Math. Phys. 71, 29 (2020). https://doi.org/10.1007/s00033-020-1250-8
Received:
Revised:
Published:
DOI: https://doi.org/10.1007/s00033-020-1250-8