This shows you the differences between two versions of the page.
Both sides previous revision Previous revision Next revision | Previous revision Next revision Both sides next revision | ||
baboons [2014/06/09 17:36] cook |
baboons [2014/06/09 17:39] cook |
||
---|---|---|---|
Line 21: | Line 21: | ||
- The mean life of the decaying particle X -> 2n (some magic decay. Not very physical, probably. But hey, we don't actually know what WIMPS are). | - The mean life of the decaying particle X -> 2n (some magic decay. Not very physical, probably. But hey, we don't actually know what WIMPS are). | ||
- | |||
- The energy of these neutrons (although if it is high enough, it may not matter too much?) | - The energy of these neutrons (although if it is high enough, it may not matter too much?) | ||
- | |||
- The abundance of X. | - The abundance of X. | ||
- | |||
- n interaction rates with every other nucleus. | - n interaction rates with every other nucleus. | ||
Line 32: | Line 29: | ||
Reference Papers: | 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]] | ||
**Logbook** | **Logbook** |