Appendix 1
The first Einstein field equation and its solutions
The Einstein-Hilbert equation for empty space (i.e., Einstein vacuum) has the form of equation (1) for
where
is the scalar curvature;
is Ricci tensor;
is Christoffel symbols.
Combining Eq.s (1.A1) with the contravariant components of the metric tensor
, we obtain
where
is the number of space dimensions.
For any
n-dimensional space (except for
n = 2), equality (2.A1) can be satisfied only for
R = 0. Therefore, for
n = 4, Eq. (1.A1) takes the simplest form
We will call this equation the first Einstein vacuum equation, and it is an expression of the conservation laws, since
In this case, the solutions of Eq.s (3.A1) describe the metric-dynamic state of stable vacuum formations.
Einstein wrote [19]: “The equation of gravity for empty space is the only rationally substantiated case of field theory that can claim to be rigorous.”
Solutions of the Eq.s (3.A1) are considered in many works on modern differential geometry and general relativity. However, none of the publications known to the author discusses the relationship between various solutions of this equations, so we will consider it in sufficient detail.
Solutions to Eq.s (3.A1) are sought in a spherical coordinate system in the form of metrics:
where
ν and
λ are the required functions of
t and
r.
As a result of substitution of the covariant and contravariant components of the metric tensor from the metric (4.A1) into Eq. (3.A1) for the stationary (i.e., time-independent) state of the "vacuum", a system of three equations is obtained [20]:
The differential Eq. (7.A1) has three solutions:
where h1, h2, h3 are integration constants.
Eq. (8.A1) also has three solutions:
where
rb is the integration constant (the radius of the spherical volume).
For h1 = 1, h2 = rb and h3 = 0, the solutions of Eq.s (7.A1) and (8.A1) coincide.
Substituting three possible solutions (10.A1) into the metric (4.A1) we get three metrics with the same signature (+ – – –):
Performing similar operations with the components of the metric tensor from the metric (5.A1), we obtain three more metrics that also satisfy Eq.s (3.A1), but with the opposite signature (– + + +):
Irreducible into each other metrics (11.A1) – (16.A1) will be called generalized Schwarzschild metrics.
Metrics (11.A1) – (16.A1) describe the metric-dynamic state of the same vacuum region, therefore it is proposed to consider various options for averaging them, despite the fact that Eq.s (3.A1) is non-linear and, as a rule, in such cases, the sum of his decisions is not his own decision.
If the centers of the metrics (11.A1) – (13.A1) and (14.A1) – (16.A1) are aligned, then it is obvious that their sum is equal to zero
is also a trivial solution of the vacuum Eq.s (3.A1).
Thus, contrary to expectations, the addition of six metrics (11.A1) – (16.A1) led to an additional solution to Eq. (3.A1).
Consider now the arithmetic mean of two metrics (11.A1) and (12.A1)
The distance between two points
r1 and
r2 along the length with the signature (+ – – –) in general relativity is determined by the expression
in the case of substitution
from the averaged metric (20.A1), we obtain
Let’s first find the value of the segment between the points r1= rb and r2 = ∞:
The length of this segment is equal to the radius of the cavity rb, and the imaginary nature of this result indicates that there is no "vacuum" in the cavity. Outside this cavity from r1= rb to r2 = ∞ we have
In the absence of vacuum deformation, the distance between the points r2 = ∞ and r1 = rb is equal ∞ – rb, and in the case under consideration it is equal to (24.A1). The difference between these segments is approximately equal to
This result shows that the average vacuum extension on the segment ]rb, ∞[ is compressed by the value ~ rb, in all radial directions due to the fact that it is displaced from the cavity with radius (25.A1). This result is similar to an air bubble in a liquid (Figure 2.A.1).
The difference between the initial (non-curved) state of a local area of vacuum and its actual (curved) state is determined by the difference [21]
where
are the components of the metric tensor of the non-curved vacuum from the metric (13.A1).
Figure 2.A1.
Air bubble in liquid
Figure 2.A1.
Air bubble in liquid
Figure 3.A1.
Graph of the function lr(–) – the relative elongation of the vacuum in the outer shell surrounding the spherical cavity. The calculation was performed at rb = 2, using the software MathCad 15
Figure 3.A1.
Graph of the function lr(–) – the relative elongation of the vacuum in the outer shell surrounding the spherical cavity. The calculation was performed at rb = 2, using the software MathCad 15
The relative elongation of the vacuum region in this case is [21]
whence it follows [21]
and
The uncarved state of the vacuum section under consideration is given by the metric (13.A1), therefore, substituting the components gii0(–) and gii(–), respectively, from (13.A1) and (20.A1) into (29.A1), we obtain the relative elongation of the vacuum in each radial direction in the region from rb to ∞ (30.A1)
The graph of the function lr(–) (30.A1) is shown in Figure 3.A1. For r = rb, this function tends to infinity, and for r < rb it becomes imaginary.
Here we will not discuss the question: – What is inside the cavity with radius rb, if the vacuum is displaced from there? When considering the second and third Einstein vacuum equations (8) and (43), this problem will be solved by itself.
Thus, averaging the metrics (11.A1) and (11.A1) leads to a metric-dynamic description of a stable vacuum formation of the "air bubble in liquid" (see Figure 3.A1) type, while these metrics alone do not lead to such results.
Averaging the metrics (14.A1) and (15.A1) allows you to get similar results, but with the opposite signature