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The concept of curvature in physics through various examples, including circles, spheres, and the mercator projection. It discusses how curvature depends on perspective and dimension, and introduces the concept of intrinsic curvature. The document also explains how general relativity relates gravitational effects to curvature in space and time.
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General relativity, III
Curvature
The “curvature” of a function f ( x ) at any point x is defined as
d^2 f dx^2 at that point; the second derivative measures how much f deviates from being a straight-line. For functions of more than one variable, “curvature” has a less obvious meaning. Curvature, in part, involves a point of view. For example, if we look at a circle drawn on a sheet of paper it appears to be clearly “curved.” In this case, we say the circle is “embedded” in a 2-dimensional plane. On the other hand, we can equally well embed the circle in 1-dimension. To do this, every point of the circle is mapped onto a straight-line segment whose ends are “identified” with each other. So is the circle curved or straight? In particular, what if we were 1-dimensional bugs confined to crawl around in the 1-dimensional world of the circle; would we say our world was curved or straight?
As another example, let’s consider again the Mercator projection (MP) discussed in GR 2. The MP is a planar representation of the latitude and longitude coordinates that identify any point on the surface of a sphere. It is an embedding of the sphere’s 2D surface in a 2-dimensional plane, as in the figure to the right. In 2D, the sphere’s latitude and longitude coordinate system certainly looks like a nice, flat, rectangular grid. On the other hand, when viewed from “outside”—that is, when embedded in 3D—the sphere’s surface is clearly curved. So if we were 2D bugs confined to crawl around on the surface of a sphere would we say our world was curved or flat?
Consider one more example, namely, a torus (or “doughnut”)—seen to the right. When viewed from the perspective of 3D, the torus certainly seems curved. As for the sphere, we can label any point on the surface of the torus with two coordinates (suggested by the curved arrows on the figure)—an angle saying how far around the outside the point is, and a second saying how far around a circular cross-section it is. If we embed this coordinate system in a plane it looks like a nice, flat, rectangular grid. So, once more, if we were 2D bugs confined to crawl around on the surface of a torus would we say our world was curved or flat?
As for the circle in 1D, both the MP for a sphere and the equivalent projection for a torus are planar representations that have “identified points.” In the MP figure above, for example, the “north pole” is the set of points with different longitude coordinates but all with latitude = 90˚. Similarly, the “south pole” consists of all points with latitude = −90˚. The “anti-meridian” is the set of all points with longitude = 180˚ or −180˚. Every point on the 180˚ anti-meridian is also on the - 1 80˚ anti-meridian. A similar situation is true for the 2D embedding of a torus. Identification of points guarantees the surface in question is closed (that is, you warp around to where you started if you crawl far enough) but it doesn’t say anything about curvature. The important issue for bugs crawling around on a surface is whether when they start off traveling parallel to one another they eventually collide despite each crawling in the straightest paths possible. That won’t happen (by definition) if the surface is flat but might if the surface is curved. Such curvature is called “intrinsic” and has nothing to do with the shape of the surface when embedded in different dimensional spaces. Using the criterion for flatness of nonintersecting “parallel” paths, we conclude that a sphere really is curved, but that a torus is not. The convergence (or not) of
parallel paths on most surfaces (including a circle) is not easily visualized. What is needed is a formal calculation whose result tells us the answer.
There are several ways of measuring intrinsic curvature. All involve taking second derivatives of some function in its many independent variable “directions.” The definition of space-time curvature used in general relativity (“Riemannian curvature”) focuses on how s-t intervals are measured in some system of time and space coordinates. In special relativity, the s-t interval between two nearby events—also
( x, y, z ) are used. It is straightforward to show that the same line element is
μ , != 0
3
(^) q^ μis a general s-t coordinate with the superscript taking on one of
four possible values, 0 through 3. The 16 quantities
g μ!together constitute the so-called “metric.” (A geeky bit: the metric is a tensor of rank two—that is, it has two subscripts, as opposed to a vector, which has one, or a scalar, which has none.) The Riemannian curvature is a linear combination of the various second derivatives of g μν.
be q^0 = T , q^1 = x , q^2 = y , q^3 = z , and the metric components are then gTT =! 1 , gxx = 1 , gyy = 1 , gzz = 1 ,
coordinates can be taken to be q^0 = T , q^1 = r , q^2 =! , q^3 = "and gTT =! 1 , grr = 1 , g "" = r^2 , g ## = r^2 sin^2 ", with all others being = 0. It’s clear that the first of these metrics has all zeroes for its second derivatives and therefore corresponds to zero curvature. The second metric has some second derivatives that don’t vanish. On the other hand, though it’s a bit of a mess to do, combining these derivatives in the definition of the Riemannian curvature also produces zero. Thus, even though the line element for a special relativistic inertial observer in spherical coordinates looks like there should be curvature, there isn’t any.
Einstein’s theory of gravity
Einstein’s version of gravity says that gravitational effects can be understood as curvature in space and time. A test particle feely falling through space-time travels on the straightest world line—a “geodesic”—it can; it feels no gravitational force. But, geodesic world lines of nearby particles can converge or diverge because of gravitational curvature.
Einstein’s gravitational field equations are similar in many respects to Maxwell’s equations for electromagnetism. Like Maxwell’s equations, they are second order partial differential equations. Solutions to Maxwell’s equations are electric and magnetic fields; solutions to Einstein’s equations are gravitational fields (though disguised as components of the metric, g μν). Both Maxwell and Einstein relate their respective fields to “sources.” For Maxwell the sources are stationary and moving charges (currents). For Einstein the sources include stationary and moving masses. In both theories, moving sources make fields—that is, a kind of “magnetism.” In both theories, accelerating sources make fields that propagate—that is, electromagnetic and gravitational waves.
But there is also a significant difference between Maxwell and Einstein. Electromagnetic fields do not carry charge—the stuff that makes them. When two electromagnetic waves overlap, they linearly