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--- examples_aswns_kepler [2022/08/16 21:54]
theoastro [A first Test]
+++ examples_aswns_kepler [2022/08/16 22:02] (current)
theoastro [Plotting your results]
@@ Line 64: / Line 64: @@
 This was simply the first step of the iteration, and you see that the code is continuously increasing the mass and trying to find the maximum mass that you can reach the Kepler limit.
-The final results will be written in the file that you provided, by default this would be kepler.dat. The individual columns refer to:  the central density, axial Omega, the corresponding error flag (0 means no error), the gravitational mass in Msun, the baryonic mass in Msun, total stellar entropy, the angular momentum, the rotational energy, the equatorial omega, the Keplerian Omega, the equatorial radius in Msun, the equatorial radius in km, radius at the pole in Msun, the disk mass, dm/drho
+The final results will be written in the file that you provided, by default this would be kepler.dat. The individual columns refer to:
+     * the central density
+    * axial Omega
+    * the corresponding error flag (0 means no error)
+    * the gravitational mass in Msun
+    * the baryonic mass in Msun
+    * the proper mass
+    * total stellar entropy,
+    * the angular momentum
+    * the rotational energy
+    * the equatorial omega,
+    * the Keplerian Omega
+    *  the equatorial radius in Msun,
+    * the equatorial radius in km
+    *  radius at the pole in Msun
+    *  the disk mass
+    * the derivative dm/drho
 ==== Plotting your results ====
+Based on the result in kepler.dat, you could check your results. One straight forward way would be to look at m(rho) and plot this with gnuplot, e.g.,
+gnuplot
+gnuplot> plot 'kepler.dat' u 1:4 w l
+which gives you the following plot of the gravitational mass as a function of the central density.
+{{aswns_kepler_simple.png}}

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