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Stress-energy tensor, force density and local balance on flat spacetime
Definition
Let be the affine Minkowski model (Oriented time-oriented affine Minkowski space (the spacetime primitives)), fix an independent numerical parameter , and let be a nonempty open set.
(a) A stress-energy tensor on of class , (with meaning continuous), is a symmetric type- tensor field on in the sense of C^k tensor fields on affine Minkowski space and their inertial components: at every the map is bilinear and symmetric, so in every inertial chart its components satisfy (Transformation of tensor, covector, derivative and current components under affine Lorentz maps,(iii)).
(b) In each inertial chart of the model (Inertial frames and inertial charts of the affine Minkowski model) define the component families , and . These are numerical component and scaling conventions involving the fixed positive number ; their transformation behaviour is inherited from and no physical units or measurement interpretation form part of this mathematical definition.
(c) When , the four-force density of is the field whose inertial components are , where are the coordinate partial derivatives of Directional derivatives and partial derivatives of a map and the sum over is the standard contraction of a contravariant index with a coordinate derivative. The components transform as a vector, so is a well-defined vector field on independent of the inertial chart: under an inertial transition the components satisfy (Transformation of tensor, covector, derivative and current components under affine Lorentz maps,(iv)), which is exactly the vector transformation law of clause (i) applied to the components . For one says that is locally conserved, or balanced, on when on , and that is balanced against the four-force density when .
(d) The definition asserts no conservation of any prescribed symmetric field : whether a given is conserved, whether it arises from an action or a matter model, and whether any of its integrals over a slice converges are separate hypotheses stated elsewhere. No choice principle is used. For a merely continuous tensor () the component conventions and pointwise contractions of (b) are defined, while the divergence, the four-force density and the balance terminology of (c) require the additional hypothesis; no derivative of a merely continuous field is asserted.
Remarks
The symmetry condition in (a) is chart-independent by the rank-two component law (Transformation of tensor, covector, derivative and current components under affine Lorentz maps,(iii)): if in one inertial chart, then in every other. The constants of (b) are numerical component conventions only; the physical readings of such components — energy density, momentum density, stress, force density — are model premises adopted separately in Adopted continuum matter models, evolution equations and observer readings and used in Local conservation of the adopted matter stress-energy tensors. Nothing in this definition requires the metric contraction to have a sign, requires any energy condition, or asserts that a locally conserved field is the total stress-energy of an isolated system.
Depends on
Oriented time-oriented affine Minkowski space (the spacetime primitives)
C^k tensor fields on affine Minkowski space and their inertial components
Transformation of tensor, covector, derivative and current components under affine Lorentz maps
Directional derivatives and partial derivatives of a map
Lorentz forms of inertia (3,1,0) on a 4-dimensional real vector space
Inertial frames and inertial charts of the affine Minkowski model
Dependency tree · 2 levels
Sources
- B. Crowell, Special Relativity, revision 2020-12-10 (author-published undergraduate textbook, 246 PDF pages); signature (+---) converted to (-+++) and c = 1 formulas converted to x^0 = c t; Chapter 9 pp. 179-197: 9.1 pp. 179-182 (current vector, flux, charge conservation), 9.2 pp. 183-191 (stress-energy tensor, conservation and flux, symmetry, dust, rank-2 transformation law, pressure, perfect fluid, worked examples, energy conditions), 9.3 pp. 192-197 (Gauss's theorem, integral conservation laws, the energy-momentum vector, angular momentum); the printed 9.2.8 dominant energy condition p. 191 has the defective |P| > rho and is not used
- D. Tong, General Relativity, University of Cambridge Part III Mathematical Tripos (Michaelmas Term 2019); c = 1 formulas converted to x^0 = c t; 4.5.1-4.5.5 printed pp. 181-191: scalar-field action (4.42)-(4.43) and equation of motion, Hilbert energy-momentum tensor (4.46), diffeomorphism invariance and conservation (4.50), flat-space Noether form, scalar tensor (4.51), Maxwell tensor (4.52), perfect fluid (4.53) with conservation equations (4.54)-(4.55), and the flat-space conserved-charge box argument of 4.5.5
- S. M. Carroll, Lecture Notes on General Relativity, arXiv:gr-qc/9712019v1 (1997), Chapter 1 printed pp. 28-30 (energy-momentum tensor, dust T^{mu nu}=rho U^mu U^nu (1.106), perfect fluid (1.107)-(1.110), scalar and Maxwell tensors (1.111)-(1.112), conservation (1.113) with the remark that the proof follows from each matter model's equations of motion) and Chapter 5 printed pp. 138-139 (on-shell conservation from diffeomorphism invariance with compact-support variations, (5.34)-(5.38))