Notes on Relativity and Cosmology - Physics Department, UCSB
Notes on Relativity and Cosmology - Physics Department, UCSB Notes on Relativity and Cosmology - Physics Department, UCSB
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
- Page 150 and 151: 150 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 152 and 153: 152 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 154 and 155: 154 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 156 and 157: 156 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 158 and 159: 158 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 160 and 161: 160 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 162 and 163: 162 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 164 and 165: 164 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 166 and 167: 166 CHAPTER 6. DYNAMICS: ENERGY AND
- Page 168 and 169: 168 CHAPTER 7. RELATIVITY AND THE G
- Page 170 and 171: 170 CHAPTER 7. RELATIVITY AND THE G
- Page 172 and 173: 172 CHAPTER 7. RELATIVITY AND THE G
- Page 174 and 175: 174 CHAPTER 7. RELATIVITY AND THE G
- Page 176 and 177: 176 CHAPTER 7. RELATIVITY AND THE G
- Page 178 and 179: 178 CHAPTER 7. RELATIVITY AND THE G
- Page 180 and 181: 180 CHAPTER 7. RELATIVITY AND THE G
- Page 182 and 183: 182 CHAPTER 7. RELATIVITY AND THE G
- Page 184 and 185: 184 CHAPTER 7. RELATIVITY AND THE G
- Page 186 and 187: 186 CHAPTER 7. RELATIVITY AND THE G
- Page 188 and 189: 188 CHAPTER 7. RELATIVITY AND THE G
- Page 190 and 191: 190 CHAPTER 7. RELATIVITY AND THE G
- Page 192 and 193: 192 CHAPTER 7. RELATIVITY AND THE G
- Page 194 and 195: 194 CHAPTER 8. GENERAL RELATIVITY A
- Page 196 and 197: 196 CHAPTER 8. GENERAL RELATIVITY A
- Page 198 and 199: 198 CHAPTER 8. GENERAL RELATIVITY A
- Page 202 and 203: 202 CHAPTER 8. GENERAL RELATIVITY A
- Page 204 and 205: 204 CHAPTER 8. GENERAL RELATIVITY A
- Page 206 and 207: 206 CHAPTER 8. GENERAL RELATIVITY A
- Page 208 and 209: 208 CHAPTER 8. GENERAL RELATIVITY A
- Page 210 and 211: 210 CHAPTER 8. GENERAL RELATIVITY A
- Page 212 and 213: 212 CHAPTER 8. GENERAL RELATIVITY A
- Page 214 and 215: 214 CHAPTER 8. GENERAL RELATIVITY A
- Page 216 and 217: 216 CHAPTER 8. GENERAL RELATIVITY A
- Page 218 and 219: 218 CHAPTER 8. GENERAL RELATIVITY A
- Page 220 and 221: 220 CHAPTER 8. GENERAL RELATIVITY A
- Page 222 and 223: 222 CHAPTER 8. GENERAL RELATIVITY A
- Page 224 and 225: 224 CHAPTER 8. GENERAL RELATIVITY A
- Page 226 and 227: 226 CHAPTER 8. GENERAL RELATIVITY A
- Page 228 and 229: 228 CHAPTER 9. BLACK HOLES of gravi
- Page 230 and 231: 230 CHAPTER 9. BLACK HOLES However,
- Page 232 and 233: 232 CHAPTER 9. BLACK HOLES require
- Page 234 and 235: 234 CHAPTER 9. BLACK HOLES √ dr r
- Page 236 and 237: 236 CHAPTER 9. BLACK HOLES Future I
- Page 238 and 239: 238 CHAPTER 9. BLACK HOLES r = R s
- Page 240 and 241: 240 CHAPTER 9. BLACK HOLES r < R s
- Page 242 and 243: 242 CHAPTER 9. BLACK HOLES this: Fi
- Page 244 and 245: 244 CHAPTER 9. BLACK HOLES Well, ou
- Page 246 and 247: 246 CHAPTER 9. BLACK HOLES finite p
- Page 248 and 249: 248 CHAPTER 9. BLACK HOLES r = R s
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