Komar mass
The Komar mass (named after Arthur Komar) of a system is one of several formal concepts of mass that are used in general relativity. The Komar mass can be defined in any stationary spacetime, which is a spacetime in which all the metric components can be written so that they are independent of time. Alternatively, a stationary spacetime can be defined as a spacetime which possesses a timelike Killing vector field. The following discussion is an expanded and simplified version of the motivational treatment in (Wald, 1984, pg 288). Motivation. Consider the Schwarzschild metric. Using the Schwarzschild basis , a for the Schwarzschild metric, one can find that the radial acceleration required to hold a test mass stationary at a Schwarzschild coordinate of "r" is: Because the metric is static, there is a well-defined meaning to "holding a particle stationary". Interpreting this acceleration as being due to a "gravitational force", we can then compute the integral of normal acceleration multiplied by area to get a "Gauss law" integral of: While this approaches a constant as r approaches infinity, it is not a constant independent of "r". We are therefore motivated to introduce a correction factor to make the  above integral independent of the radius "r" of the enclosing shell. For the Schwarzschild metric, this correction factor is just formula_3, the "red-shift" or "time dilation" factor at distance "r". One may also view this factor as "correcting" the local force to the "force at infinity", the force that an observer at infinity would need to apply through a string to hold the particle stationary. (Wald, 1984). To proceed further, we will write down a line element for a static metric. where "g" and the quadratic form are functions only of the spatial coordinates "x", "y", "z" and are  not functions of time. In spite of our choices of variable names, it should not be assumed that our coordinate system is Cartesian. The fact that none of the metric coefficients are functions of time makes the metric stationary: the additional fact that there are no "cross terms" involving both time and space components (such as "dx dt") make it static. Because of the simplifying assumption that some of the metric coefficients are zero, some of our results in this motivational treatment will not be as general as they could be. In flat space-time, the proper acceleration required to  hold station is formula_5, where "u" is the 4-velocity of our hovering particle and tau is the proper time. In curved space-time, we must take the covariant derivative. Thus we compute the acceleration vector as: where "u" is a unit time-like vector such that "u u" = -1. The component of the acceleration vector normal to the surface is where N is a unit vector normal to the surface. In a Schwarzschild coordinate system, for example, we find that as expected - we have simply re-derived the previous results presented in a frame-field in a coordinate  basis. We define so that in our Schwarzschild example: formula_11 We can, if we desire, derive the accelerations "a" and the adjusted "acceleration at infinity" "a" inf from a scalar potential Z, though there is not necessarily any particular advantage in doing so. (Wald 1984, pg 158, problem 4) We will demonstrate that integrating the normal component of the "acceleration at infinity" "a" inf over a bounding surface will give us a quantity that does not depend on the shape of the enclosing sphere, so that we can calculate the mass enclosed by a sphere by the integral To make  this demonstration, we need to express this surface integral as a volume integral. In flat space-time, we would use Stokes theorem and integrate formula_15 over the volume. In curved space-time, this approach needs to be modified slightly. Using the formulas for electromagnetism in curved space-time as a guide, we write instead. where F plays a role similar to the "Faraday tensor", in that formula_17 We can then find the value of "gravitational charge", i.e. mass, by evaluating formula_18 and integrating it over the volume of our sphere. An alternate approach would be to use differential forms, but  the approach above is computationally more convenient as well as not requiring the reader to understand differential forms. A lengthy, but straightforward (with computer algebra) calculation from our assumed line element shows us that Thus we can write In any vacuum region of space-time, all components of the Ricci tensor must be zero. This demonstrates that enclosing any amount of vacuum will not change our volume integral. It also means that our volume integral will be constant for any enclosing surface, as long as we enclose all of the gravitating mass inside our surface. Because Stokes theorem guarantees that  our surface integral is equal to the above volume integral, our surface integral will also be independent of the enclosing surface as long as the surface encloses all of the gravitating mass. By using Einstein's Field Equations letting u=v and summing, we can show that "R" = -8π"T". This allows us to rewrite our mass formula as a volume integral of the stress–energy tensor. where Komar mass as volume integral - general stationary metric. To make the formula for Komar mass work for a general stationary metric, regardless of the choice of coordinates, it must be modified  slightly. We will present the applicable result from (Wald, 1984 eq 11.2.10) without a formal proof. where Note that formula_24 replaces formula_27 in our motivational result. If none of the metric coefficients formula_28 are functions of time, formula_29 While it is not "necessary" to choose coordinates for a stationary space-time such that the metric coefficients are independent of time, it is often "convenient". When we chose such coordinates, the time-like Killing vector for our system formula_30 becomes a scalar multiple of a unit coordinate-time vector formula_31 i.e. formula_32 When this is the case, we can rewrite our  formula as Because formula_34 is by definition a unit vector, K is just the length of formula_24, i.e. K = formula_36. Evaluating the "red-shift" factor K based on our knowledge of the components of formula_30, we can see that K = formula_3. If we chose our spatial coordinates so that we have a locally Minkowskian metric formula_39 we know that With these coordinate choices, we can write our Komar integral as While we can't choose a coordinate system to make a curved space-time globally Minkowskian, the above formula provides some insight into the meaning of the Komar  mass formula. Essentially, both energy and pressure contribute to the Komar mass. Furthermore, the contribution of local energy and mass to the system mass is multiplied by the local "red shift" factor formula_42 Komar mass as surface integral - general stationary metric. We also wish to give the general result for expressing the Komar mass as a surface integral. The formula for the Komar mass in terms of the metric and its Killing vector is (Wald, 1984, pg 289, formula 11.2.9) where formula_44 are the Levi-civita symbols and formula_45 is the Killing vector of our stationary metric, normalized so that  formula_25 at infinity. The surface integral above is interpreted as the "natural" integral of a two form over a manifold. As mentioned previously, if none of the metric coefficients formula_28 are functions of time, formula_48