[Commits] [svn:einsteintoolkit] www/about/gallery/tov/ (Rev. 1558)

[barry.wardell at gmail.com]

User: barry.wardell
Date: 2016/06/05 07:38 PM

Modified:
 /about/gallery/tov/
  index.php

Log:
 too example: spelling and grammar corrections

File Changes:

Directory: /about/gallery/tov/
==============================

File [modified]: index.php
Delta lines: +4 -4
===================================================================
--- about/gallery/tov/index.php	2016-06-06 00:33:08 UTC (rev 1557)
+++ about/gallery/tov/index.php	2016-06-06 00:38:01 UTC (rev 1558)
@@ -3,12 +3,12 @@
 
   <p>This simulation shows how to evolve a stable, single neutron star. It uses a TOV solution
      as initial data and follows the initial (numerical) perturbations, writing the maximum
-     density to disk. What can be seen is that the oscillates for a few cycles (only very
-     slitely because the solution is stationary and the induced numerical perturbation is small),
+     density to disk. What can be seen is that the star oscillates for a few cycles (only very
+     slightly because the solution is stationary and the induced numerical perturbation is small),
      before numerical errors due to the lack of resolution spoil the results. The size of this
      simulation is intentionally kept as small as possible, thus the resolution is about as low
-     as youcan go without loosing any confidence in at least quantitatively correct results.
-     It is intended to be used as quick examples in lectures, workshops or summer schools where
+     possible without loosing any confidence in at least quantitatively correct results.
+     It is intended to be used as quick example in lectures, workshops or summer schools where
      both time and computational power are typically scarce.</p>
   <table>
    <tr><th>Parameter file</th><td><a href="tov.par">tov.par</a></td></tr>