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wiki:core_collapse_supernovae_neutron_star_mergers_and_grbs_hix_ott [2012/10/10 10:51]
nucastro Rauscher made these additions
wiki:core_collapse_supernovae_neutron_star_mergers_and_grbs_hix_ott [2013/01/10 17:47] (current)
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   * Astrophysical simulations need consistent treatment of masses and rates with frequent updates.   * Astrophysical simulations need consistent treatment of masses and rates with frequent updates.
    
-  * Rauscher: Since the site of the r-process is unknown, parameterized studies need to explore wide ranges of conditions (e.g., low Ye in NS mergers moves the path close to dripline, beta-decays,​ 2neutron captures and direct reactions at dripline become relevant) also nuclear physics has to be known from stability to dripline (unfortunately).+  * Rauscher: Since the site of the r-process is unknown, parameterized studies need to explore wide ranges of conditions ​and trajectories ​(e.g., low Ye in NS mergers moves the path close to dripline, beta-decays,​ 2neutron captures and direct reactions at dripline become relevant) also nuclear physics has to be known from stability to dripline (unfortunately).
   * Meyer: Parameterized studies may not provide unique set of conditions when compared to r-abundances;​ neutron-to-seed ratio critical but, e.g., different trajectories etc may yield different conditions (and position of r-path).   * Meyer: Parameterized studies may not provide unique set of conditions when compared to r-abundances;​ neutron-to-seed ratio critical but, e.g., different trajectories etc may yield different conditions (and position of r-path).
  
wiki/core_collapse_supernovae_neutron_star_mergers_and_grbs_hix_ott.txt ยท Last modified: 2013/01/10 17:47 (external edit)