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 In case (1), this effect is important only if the decay channels are relativistic, thus adding a lot of entropy into the universe. In this project, we will consider the injection of neutrons, so we will not consider this effect.
+It is thus the goal of this project to investigate the effect of the injection of non-thermal neutrons on the light element abundances.
 **Key parameters: **
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   - The abundance of X.
   - n interaction rates with every other nucleus.
+  - Mass of the WIMP. Chosen to be 100 GeV, based on the wikipedia WIMP entry, the font of all wisdom.
+This figure:
+{{::cdms_parameter_space_2004.png?600|}}
+from CDMS in 2004 suggests that this value isn't too far off.
 Reference Papers:
-Cyburt et. al. 2009 Nucleosynthesis Constraints on a Massive Gravitino in Neutralino Dark Matter Scenario [[http://arxiv.org/pdf/0907.5003v1.pdf]]
+Cyburt et. al. 2009. Nucleosynthesis Constraints on a Massive Gravitino in Neutralino Dark Matter Scenario [[http://arxiv.org/pdf/0907.5003v1.pdf]]
+Kamionkowski 1994. Diffuse Gamma Rays from WIMP Decay and Annihilation [[http://arxiv.org/pdf/astro-ph/9404079v1.pdf]]
+Pierre Salati, 2014. Dark Matter Annihilation in the Universe [[http://arxiv.org/pdf/1403.4495.pdf]]
 **Logbook**

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