На русском языке

Pressure field tensor

The pressure field tensor is an antisymmetric tensor describing the pressure field and consisting of six components. Tensor components are at the same time components of the two three-dimensional vectors – pressure field strength and the solenoidal pressure vector. With the pressure field tensor the pressure stress-energy tensor, the pressure field equations and pressure force in matter are defined. Pressure field is a component of general field.

Contents

  • 1 Definition
  • 2 Expression for the components
  • 3 Properties of tensor
  • 4 Pressure field
  • 5 Covariant theory of gravitation
    • 5.1 Action and Lagrangian
    • 5.2 Pressure stress-energy tensor
    • 5.3 Generalized velocity and Hamiltonian
  • 6 See also
  • 7 References
  • 8 External links

Definition

Expression for the pressure field tensor can be found in papers by Sergey Fedosin, [1] where the tensor is defined using 4-curl:

f_{\mu \nu} = \nabla_\mu \pi_\nu - \nabla_\nu \pi_\mu = \frac{\partial \pi_\nu}{\partial x^\mu} - \frac{\partial \pi_\mu}{\partial x^\nu}.\qquad\qquad (1)

Here pressure 4-potential ~ \pi_\mu   is given by:

~\pi_\mu = \left( \frac {\wp }{ c}, -\mathbf{\Pi } \right),

where ~\wp   is the scalar potential, ~ \mathbf{\Pi }   is the vector potential of pressure field, ~ c  – speed of light.

Expression for the components

The pressure field strength and the solenoidal pressure vector are found with the help of (1):

~ C_i= c (\partial_0 \pi_i -\partial_i \pi_0),

 

~ I_k= \partial_i \pi_j -\partial_j \pi_i ,

and the same in vector notation:

~\mathbf{C}= -\nabla \wp - \frac{\partial \mathbf{\Pi }} {\partial t},

 

~\mathbf{I }= \nabla \times \mathbf{\Pi }.

The pressure field tensor in Cartesian coordinates consists of the components of these vectors:

~ f_{\mu \nu}= \begin{vmatrix} 0 & \frac {C_x}{ c} & \frac {C_y}{ c} & \frac {C_z}{ c} \\ -\frac {C_x}{ c} & 0 & - I_{z} & I_{y} \\ -\frac {C_y}{ c} & I_{z} & 0 & -I_{x} \\ -\frac {C_z}{ c}& -I_{y} & I_{x} & 0 \end{vmatrix}.

The transition to the pressure field tensor with contravariant indices is carried out by multiplying by double metric tensor:

~ f^{\alpha \beta}= g^{\alpha \nu} g^{\mu \beta} f_{\mu \nu}.

In the special relativity, this tensor has the form:

~ f^{\alpha \beta}= \begin{vmatrix} 0 &- \frac {C_{x}}{ c} & -\frac {C_{y}}{ c} & -\frac {C_{z}}{ c} \\ \frac {C_{x}}{ c} & 0 & - I_{z} & I_{y} \\ \frac {C_{y}}{ c}& I_{z} & 0 & -I_{x} \\ \frac {C_{z}}{ c}& -I_{y} & I_{x} & 0 \end{vmatrix}.

To convert the components of the pressure field tensor from one inertial system to another we must take into account the transformation rule for tensors. If the reference frame K'  moves with an arbitrary constant velocity ~ \mathbf {V}   with respect to the fixed reference system K, and the axes of the coordinate systems parallel to each other, the pressure field strength and the solenoidal pressure vector are converted as follows:

\mathbf {C}^\prime = \frac {\mathbf {V}}{V^2} (\mathbf {V}\cdot \mathbf {C}) + \frac {1}{\sqrt{1 - {V^2 \over c^2}}} \left(\mathbf {C}-\frac {\mathbf {V}}{V^2} (\mathbf {V}\cdot \mathbf {C}) + [\mathbf {V} \times \mathbf {I }] \right),

 

\mathbf {I }^\prime = \frac {\mathbf {V}}{V^2} (\mathbf {V}\cdot \mathbf {I }) + \frac {1}{\sqrt{1 - {V^2 \over c^2}}} \left(\mathbf {I }-\frac {\mathbf {V}}{V^2} (\mathbf {V}\cdot \mathbf {I }) - \frac {1}{ c^2} [\mathbf {V} \times \mathbf {C}] \right).

Properties of tensor

  • ~ f_{\mu \nu}  is the antisymmetric tensor of rank 2, it follows from this condition ~ f_{\mu \nu} =-f_{\nu \mu} . Three of the six independent components of the pressure field tensor associated with the components of the pressure field strength  ~ \mathbf {C} , and the other three – with the components of the solenoidal pressure vector  ~ \mathbf {I} . Due to the antisymmetry such invariant as the contraction of the tensor with the metric tensor vanishes: ~ g^{\mu \nu} f_{\mu \nu}= f^{\mu}_\mu =0.
  • Contraction of tensor with itself  f_{\mu \nu} f^{\mu \nu}  is an invariant, and the contraction of tensor product with Levi-Civita symbol as \frac {1}{4} \varepsilon^{\mu \nu \sigma \rho} f_{\mu \nu} f_{\sigma \rho}  is the pseudoscalar invariant. These invariants in the special relativity can be expressed as follows:

f_{\mu \nu} f^{\mu \nu} = -\frac {2}{c^2} (C^2- c^2 I^2) = inv,

 

\frac {1}{4} \varepsilon^{\mu \nu \sigma \rho}f_{\mu \nu} f_{\sigma \rho} = - \frac {2}{ c } \left( \mathbf C \cdot \mathbf {I} \right) = inv.

  • Determinant of the tensor is also Lorentz invariant:

\det \left( f_{\mu \nu} \right) = \frac{4}{c^2} \left(\mathbf C \cdot \mathbf {I} \right)^{2}.

Pressure field

Through the pressure field tensor the equations of pressure field are written:

\nabla_\sigma f_{\mu \nu}+\nabla_\mu f_{\nu \sigma}+\nabla_\nu f_{\sigma \mu}=\frac{\partial f_{\mu \nu}}{\partial x^\sigma} + \frac{\partial f_{\nu \sigma}}{\partial x^\mu} + \frac{\partial f_{\sigma \mu}}{\partial x^\nu} = 0. \qquad\qquad (2)

 

~ \nabla_\nu f^{\mu \nu} = - \frac{4 \pi \sigma }{c^2} J^\mu, \qquad\qquad (3)

where J^\mu = \rho_{0} u^\mu   is the mass 4-current, \rho_{0}  is the mass density in comoving reference frame, u^\mu   is the 4-velocity, ~ \sigma is a constant.

Instead of (2) it is possible use the expression:

~ \varepsilon^{\mu \nu \sigma \rho}\frac{\partial f_{\mu \nu}}{\partial x^\sigma} = 0 .

Equation (2) is satisfied identically, which is proved by substituting into it the definition for the pressure field tensor according to (1). If in (2) we insert tensor components f_{\mu \nu} , this leads to two vector equations:

~ \nabla \times \mathbf{C} = - \frac{\partial \mathbf{I} } {\partial t} , \qquad\qquad (4)

 

~ \nabla \cdot \mathbf{I} = 0 . \qquad\qquad (5)

According to (5), the solenoidal pressure vector has no sources as its divergence vanishes. From (4) follows that the time variation of the solenoidal pressure vector leads to a curl of the pressure field strength.

Equation (3) relates the pressure field to its source in the form of mass 4-current. In Minkowski space of special relativity the form of the equation is simplified and becomes:

~ \nabla \cdot \mathbf{C} = 4 \pi \sigma \rho,

 

~ \nabla \times \mathbf{I} = \frac{1}{c^2} \left( 4 \pi \sigma \mathbf{J} + \frac{\partial \mathbf{C}} {\partial t} \right),

where ~ \rho   is the density of moving mass, ~ \mathbf{J}  is the density of mass current.

According to the first of these equations, the pressure field strength is generated by the mass density, and according to the second equation the mass current or change in time of the pressure field strength generate the circular field of the solenoidal pressure vector.

From (3) and (1) it can be obtained: [1]

~R_{{\mu \alpha }}f^{{\mu \alpha }}={\frac {4\pi \sigma }{c^{2}}}\nabla _{{\alpha }}J^{{\alpha }}=0.

 

The continuity equation for the mass 4-current  ~\nabla _{{\alpha }}J^{{\alpha }}=0  is a gauge condition that is used to derive the field equation (3) from the principle of least action.

On the other hand, the contraction of the Ricci tensor and the pressure field tensor is zero:  ~R_{{\mu \alpha }}f^{{\mu \alpha }}=0 . This is a consequence of the fact that the Ricci tensor is symmetric with respect to the permutation of its indices, while the pressure field tensor is antisymmetric, and we can write:

 

~R_{{\mu \alpha }}f^{{\mu \alpha }}=-R_{{\mu \alpha }}f^{{\alpha \mu }}=-R_{{\alpha \mu }}f^{{\alpha \mu }}=-R_{{\mu \alpha }}f^{{\mu \alpha }}=0.

 

In Minkowski space the Ricci tensor  ~R_{{\mu \alpha }}  equal to zero, the covariant derivative becomes the partial derivative, and the continuity equation becomes as follows:

 

~\partial _{{\alpha }}J^{\alpha }={\frac {\partial \rho }{\partial t}}+\nabla \cdot {\mathbf {J}}=0.

 

The wave equation for the pressure field tensor is written as: [2]

~\nabla ^{\sigma }\nabla _{\sigma }f_{{\mu \nu }}={\frac {4\pi \sigma }{c^{2}}}\nabla _{\mu }J_{\nu }-{\frac {4\pi \sigma }{c^{2}}}\nabla _{\nu }J_{\mu }+f_{{\nu \rho }}{R^{\rho }}_{\mu }-f_{{\mu \rho }}{R^{\rho }}_{\nu }+R_{{\mu \nu \lambda \eta }}f^{{\eta \lambda }}.

 

This expression uses a metric with signature  (+---)  and definition of the Ricci tensor according to. [3]  If the Ricci tensor is defined as in, [4]  then the sign of the Ricci tensors in the wave equation changes:

 

~\nabla ^{\sigma }\nabla _{\sigma }f_{{\mu \nu }}={\frac {4\pi \sigma }{c^{2}}}\nabla _{\mu }J_{\nu }-{\frac {4\pi \sigma }{c^{2}}}\nabla _{\nu }J_{\mu }-f_{{\nu \rho }}{R^{\rho }}_{\mu }+f_{{\mu \rho }}{R^{\rho }}_{\nu }+R_{{\mu \nu \lambda \eta }}f^{{\eta \lambda }}.

 

Covariant theory of gravitation

Action and Lagrangian

Total Lagrangian for the matter in gravitational and electromagnetic fields includes the pressure field tensor and is contained in the action function: [1]

~S =\int {L dt}=\int (kR-2k \Lambda - \frac {1}{c}D_\mu J^\mu + \frac {c}{16 \pi G} \Phi_{ \mu\nu}\Phi^{ \mu\nu} -\frac {1}{c}A_\mu j^\mu - \frac {c \varepsilon_0}{4} F_{ \mu\nu}F^{ \mu\nu} - 

~-{\frac {1}{c}}U_{\mu }J^{\mu }-{\frac {c}{16\pi \eta }}u_{{\mu \nu }}u^{{\mu \nu }}-{\frac {1}{c}}\pi _{\mu }J^{\mu }-{\frac {c}{16\pi \sigma }}f_{{\mu \nu }}f^{{\mu \nu }}){\sqrt {-g}}d\Sigma ,

 

where ~L   is Lagrangian, ~dt  is differential of coordinate time, ~k   is a certain coefficient, ~R   is the scalar curvature, ~\Lambda   is the cosmological constant, which is a function of the system, ~c   is the speed of light as a measure of the propagation speed of electromagnetic and gravitational interactions, ~ D_\mu   is the gravitational four-potential, ~ G    is the gravitational constant, ~ \Phi_{ \mu\nu}  is the gravitational tensor, ~ A_\mu   is the electromagnetic 4-potential, ~ j^\mu  is the electromagnetic 4-current, ~\varepsilon_0   is the electric constant, ~ F_{ \mu\nu }  is the electromagnetic tensor, ~U_{\mu }   is the 4-potential of acceleration field, ~ \eta    and  ~ \sigma   are the constants of acceleration field and pressure field, respectively, ~ u_{ \mu\nu}  is the acceleration tensor, ~ \pi_\mu   is the 4-potential of pressure field, ~ f_{ \mu\nu}  is pressure field tensor, ~\sqrt {-g}d\Sigma= \sqrt {-g} c dt dx^1 dx^2 dx^3  is the invariant 4-volume, ~\sqrt {-g}   is the square root of the determinant ~g   of metric tensor, taken with a negative sign, ~ dx^1 dx^2 dx^3   is the product of differentials of the spatial coordinates.

The variation of the action function by 4-coordinates leads to the equation of motion of a matter unit in gravitational and electromagnetic fields and pressure field: [2] [5]

~\rho _{0}A_{\beta }=\rho _{0}{\frac {Du_{\beta }}{D\tau }}=-u_{{\beta \sigma }}\rho _{{0}}u^{\sigma }=\rho _{0}{\frac {dU_{\beta }}{d\tau }}-\rho _{0}u^{\sigma }\partial _{\beta }U_{\sigma }=\Phi _{{\beta \sigma }}\rho _{0}u^{\sigma }+F_{{\beta \sigma }}\rho _{{0q}}u^{\sigma }+f_{{\beta \sigma }}\rho _{0}u^{\sigma },

where  ~A_{\beta }  is the four-acceleration of matter unit,  ~u_{\beta }  is the four-velocity with covariant index, ~\tau   is the proper time in the reference frame of the matter unit, the first term on the right is the gravitational force density, expressed with the help of the gravitational tensor, second term is the Lorentz electromagnetic force density with invariant charge density  ~\rho _{{0q}}, and the last term sets the pressure force density.

If we vary the action function by the pressure 4-potential, we obtain the equation of pressure field (3).

Pressure stress-energy tensor

With the help of pressure field tensor in the covariant theory of gravitation the pressure stress-energy tensor is constructed:

~ P^{ik} = \frac{c^2} {4 \pi \sigma }\left( -g^{im} f_{n m} f^{n k}+ \frac{1} {4} g^{ik} f_{m r} f^{m r}\right) .

The covariant derivative of the pressure stress-energy tensor determines the pressure four-force density:

~f^{\alpha }=-\nabla _{\beta }P^{{\alpha \beta }}={f^{\alpha }}_{{k}}J^{k}.

Generalized velocity and Hamiltonian

Covariant 4-vector of generalized velocity (in other notation it is generalized 4-potential) is given by:

~s_{{\mu }}=U_{{\mu }}+D_{{\mu }}+{\frac {\rho _{{0q}}}{\rho _{0}}}A_{{\mu }}+\pi _{{\mu }}.

Taking into account the generalized 4-velocity, the Hamiltonian contains the pressure field tensor and has the form:

~H = \int {( s_0 J^0 - \frac {c^2}{16 \pi G} \Phi_{ \mu\nu}\Phi^{ \mu\nu}+ \frac {c^2 \varepsilon_0}{4} F_{ \mu\nu}F^{ \mu\nu }+ \frac {c^2 }{16 \pi \eta } u_{ \mu\nu} u^{ \mu\nu}+ \frac {c^2 }{16 \pi \sigma } f_{ \mu\nu} f^{ \mu\nu} ) \sqrt {-g} dx^1 dx^2 dx^3},  

where ~ s_0   and ~ J^0  are timelike components of 4-vectors  ~ s_{\mu }   and  ~ J^{\mu } .

In the reference frame that is fixed relative to the center of momentum of system, the Hamiltonian defines the invariant energy of the system.

See also

 

References

1.        1,0 1,1 1,2 Fedosin S.G. About the cosmological constant, acceleration field, pressure field and energy. Jordan Journal of Physics. Vol. 9 (No. 1), pp. 1-30 (2016). http://dx.doi.org/10.5281/zenodo.889304.

2.        2,0 2,1 Fedosin S.G. Equations of Motion in the Theory of Relativistic Vector Fields. International Letters of Chemistry, Physics and Astronomy, Vol. 83, pp. 12-30 (2019). https://doi.org/10.18052/www.scipress.com/ILCPA.83.12.

3.        Fock V.A. The Theory of Space, Time and Gravitation. Macmillan. (1964).

4.        Landau, Lev D.; Lifshitz, Evgeny M. (1975). The Classical Theory of Fields. Vol. 2 (4th ed.). Butterworth-Heinemann. ISBN 978-0-7506-2768-9.

5.        Fedosin S.G. Two components of the macroscopic general field. Reports in Advances of Physical Sciences, Vol. 1, No. 2, 1750002, 9 pages (2017). http://dx.doi.org/10.1142/S2424942417500025.

 

External links

·       Pressure field tensor in Russian

 

Source: http://sergf.ru/tpden.htm

On the list of pages