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 | ||
group9 [2014/05/31 01:59] yuan add title and links |
group9 [2014/06/09 17:03] bliss |
||
---|---|---|---|
Line 1: | Line 1: | ||
- | ====== HAℓF ====== | + | ===== Our Project(a) on Ejecta ===== |
- | ===== Roles ===== | + | ==== Neutron Star Merger r-process ==== |
- | * **Analysis:** Alexander Dombos | + | Alison Dreyfuss, Sarah Schwartz, Julia Bliss |
- | * **Code:** Fei Yuan | + | |
- | * **Parameter:** Heiko Möller | + | |
- | ===== Topic ===== | + | **Prompt**:: Determine, using the literature, representative conditions for tidal ejection of material from neutron star mergers and for neutrino driven winds. Calculate, using the reaction network, abundance patterns for each and compare the results. Discuss why the patterns look different. |
- | //(Preliminary)// | + | == June 9 == |
- | Simulate the effects of a near-Earth supernova explosion at 10 parsec (the "kill radius") and the resulting collision of the blast with solar wind. Will the supernova reach 1 AU? How does the answer depend on the: | + | Julia:: has trajectories for temperature, density for NN merger and neutrino driven wind from [[http://arxiv.org/pdf/1307.2939v2.pdf|Korobkin work]] (specific data unavailable - part of ongoing collaboration) |
- | * supernova explosion energy, | + | Some trajectories can be found here -> http://compact-merger.astro.su.se/downloads.html |
- | * distance, and | + | |
- | * interstellar density? | + | |
- | + | ||
- | ===== External links ===== | + | |
- | + | ||
- | * [[https://github.com/xrf/talent-astro-proj1|Git repository]] | + | |
- | * [[https://docmgmt.nscl.msu.edu/share/page/site/TALENT/documentlibrary#filter=path%7C/Course7_2014/Projects/Project1/group9|Document library]] | + |