Notes on Relativity and Cosmology - Physics Department, UCSB

Notes on Relativity and Cosmology - Physics Department, UCSB Notes on Relativity and Cosmology - Physics Department, UCSB

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200 CHAPTER 8. GENERAL RELATIVITY AND CURVED SPACETIME 6 4 T 2 0 -2 -4 -6 -6 -4 -2 X 0 2 4 6 10 Note that one can move along the surface in either a timelike manner (going up the surface) or a spacelike manner (going across the surface), so that this surface does indeed represent a (1+1) spacetime. The picture above turns out to represent a particular kind of gravitational field that we will be discussing more in a few weeks. To see the similarity to the gravitational field around the earth, think about two freely falling worldlines (a.k.a. “geodesics,” the straightest possible lines) that begin near the middle of the diagram and start out moving straight upward. Suppose for simplicity that one geodesic is on one side of the fold while the second is on the other side. You will see that the two worldlines separate, just as two freely falling objects do at different heights in the earth’s gravitational field. Thus, if we drew a two-dimensional map of this curved spacetime using the reference frame of one of these observers, the results would be just like the spacetime diagram we drew for freely falling stones at different heights! This is a concrete picture of what it means to say that gravity is the curvature of spacetime. Well, there is one more subtlety that we should mention...... it is important to realize that the extra dimension we used to draw the picture above was just a crutch that we needed because we think best in flat spaces. One can in fact talk about curved spacetimes without thinking about a “bigger space” that contains points “outside the spacetime.” This minimalist view is generally a good idea, as we will discuss more in the sections below. 8 6 4 2 Y 0 -2 -4 -6 8.2 More on Curved Space Let us remember that the spacetime in which we live is fundamentally four (=3+1) dimensional and ask if this will cause any new wrinkles in our story. It

8.2. MORE ON CURVED SPACE 201 turns out to create only a few. The point is that curvature is fundamentally associated with two-dimensional surfaces. Roughly speaking, the curvature of a four-dimensional spacetime (labelled by x, y, z, t) can be described in terms of xt curvature, yt curvature, etc. associated with two-dimensional bits of the spacetime. However, this is relativity, in which space and time act pretty much the same. So, if there is xt, yt, and zt curvature, there should also be xy, yz, and xz curvature! This means that the curvature can show up even if we consider only straight lines in space (determined, for example, by stretching out a string) in addition to the effects on the motion of objects that we have already discussed. For example, if we draw a picture showing spacelike straight lines (spacelike geodesics), it might look like this: Y Two geodesics X So, curved space is as much a part of gravity as is curved spacetime. This is nice, as curved spaces are easier to visualize. Let us now take a moment to explore these in more depth and build some intuition about curvature in general. Curved spaces have a number of fun properties. Some of my favorites are: C ≠ 2πR: The circumference of a circle is typically not 2π times its radius. Let us take an example: the equator is a circle on a sphere. What is it’s center? We are only supposed to consider the two-dimensional surface of the sphere itself as the third dimension was just a crutch to let us visualize the curved two-dimensional surface. So this question is really ‘what point on the sphere is equidistant from all points on the equator?’ In fact, there are two answers: the north pole and the south pole. Either may be called the center of the sphere. Now, how does the distance around the equator compare to the distance (measured along the sphere) from the north pole to the equator? The arc running from the north pole to the equator goes 1/4 of the way around the sphere. This is the radius of the equator in the relevant sense. Of course, the equator goes once around the sphere. Thus, its circumference is exactly four times its radius. A ≠ πR 2 : The area of a circle is typically not π times the square of its radius. Again, the equator on the sphere makes a good example. With the radius

200 CHAPTER 8. GENERAL RELATIVITY AND CURVED SPACETIME<br />

6<br />

4<br />

T<br />

2<br />

0<br />

-2<br />

-4<br />

-6<br />

-6<br />

-4<br />

-2<br />

X<br />

0<br />

2<br />

4<br />

6<br />

10<br />

Note that <strong>on</strong>e can move al<strong>on</strong>g the surface in either a timelike manner (going<br />

up the surface) or a spacelike manner (going across the surface), so that this<br />

surface does indeed represent a (1+1) spacetime. The picture above turns out<br />

to represent a particular kind of gravitati<strong>on</strong>al field that we will be discussing<br />

more in a few weeks. To see the similarity to the gravitati<strong>on</strong>al field around<br />

the earth, think about two freely falling worldlines (a.k.a. “geodesics,” the<br />

straightest possible lines) that begin near the middle of the diagram <strong>and</strong> start<br />

out moving straight upward. Suppose for simplicity that <strong>on</strong>e geodesic is <strong>on</strong> <strong>on</strong>e<br />

side of the fold while the sec<strong>on</strong>d is <strong>on</strong> the other side. You will see that the two<br />

worldlines separate, just as two freely falling objects do at different heights in<br />

the earth’s gravitati<strong>on</strong>al field. Thus, if we drew a two-dimensi<strong>on</strong>al map of this<br />

curved spacetime using the reference frame of <strong>on</strong>e of these observers, the results<br />

would be just like the spacetime diagram we drew for freely falling st<strong>on</strong>es at<br />

different heights! This is a c<strong>on</strong>crete picture of what it means to say that gravity<br />

is the curvature of spacetime.<br />

Well, there is <strong>on</strong>e more subtlety that we should menti<strong>on</strong>...... it is important to<br />

realize that the extra dimensi<strong>on</strong> we used to draw the picture above was just a<br />

crutch that we needed because we think best in flat spaces. One can in fact talk<br />

about curved spacetimes without thinking about a “bigger space” that c<strong>on</strong>tains<br />

points “outside the spacetime.” This minimalist view is generally a good idea,<br />

as we will discuss more in the secti<strong>on</strong>s below.<br />

8<br />

6<br />

4<br />

2<br />

Y<br />

0<br />

-2<br />

-4<br />

-6<br />

8.2 More <strong>on</strong> Curved Space<br />

Let us remember that the spacetime in which we live is fundamentally four<br />

(=3+1) dimensi<strong>on</strong>al <strong>and</strong> ask if this will cause any new wrinkles in our story. It

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