Physics 387M - Fall 1997

Physics 387M: Relativity Theory I: Course Notes

This document will be updated throughout the course

Using the Center for Relativity SGI machines
- Brief description of available machines
- Unix notes from PHY 329 and PHY 381C.
Using Maple and GRTensor
- To use GRTensor on any of the SGI machines, start up maple (illustrated here) or xmaple, then load the tensor package and help files and initialize the package with the readlib() and grtensor() commands as shown below:
```
einstein 1> maple
    |\^/|     Maple V Release 3 (University of Texas - Austin)
._|\|   |/|_. Copyright (c) 1981-1994 by Waterloo Maple Software and the
 \  MAPLE  /  University of Waterloo. All rights reserved. Maple and Maple V
 <____ ____>  are registered trademarks of Waterloo Maple Software.
      |       Type ? for help.

> readlib(grii):
> readlib(griihelp):
> grtensor():
                          GRTensorII Version 1.58 (R3)
                                   .
                                   .
                                   .
              Defaults read from /usr/local/maple/lib/grtensor.ini
```
  Note that you can put the above three commands in your personal Maple-initialization file to save you from typing them every time you start a Maple session. The initialization file must reside in your home directory and must have the name .mapleinit. If you wish to copy mine, the command sequence
```
einstein 1> cd
einstein 2> cp ~matt/.mapleinit .
```
  should do the trick.
- Maple notes from PHY 381C.
- Maple V Home Page including links to various Maple V Web sites
- GRTensor Documentation (postscript)
- GRTensor Home Page
- Session trace illustrating basic login procedure, setting DISPLAY environment variable, starting Xmaple, and printing postscript version of Xmaple worksheet.
- Postscript version of maple worksheet illustrating computation of Riemann for flat spacetime in accelerated coordinates, as discussed in Oct 2 class.
The Schwarzschild Solution
- Postscript version of maple worksheet illustrating grtensor computations of the static spherically symmetric Einstein equations (vacuum and perfect fluid) using an orthonormal basis (following Wald, 6.1-6.2).