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====== PROJECTS ====== | ====== PROJECTS ====== | ||
- | Projects: **[[ProjectIdeas|Project Ideas]]**, **[[Project1|Project 1]]**, **[[Project2|Project 2]]** | + | Projects: **[[Projects]]**, **[[ProjectIdeas|Project Ideas]]** |
---- | ---- | ||
==== Project Ideas ==== | ==== Project Ideas ==== | ||
+ | |||
+ | == Exploding a polytropic star == | ||
+ | |||
+ | - Create a hydrostatic configuration for a polytropic star. Solutions can be derived from the Lane-Emden equation ([[http://en.wikipedia.org/wiki/Lane%E2%80%93Emden_equation|Lane-Emden equation]]). | ||
+ | - For an initial condition, increase the central pressure (and only the central point) by some factor of the hydrostatic value (just as in the Sedov Blast Wave). | ||
+ | - Evolve the star given this deposition of energy in the center of the star. | ||
+ | - Questions you can try to answer | ||
+ | * Find the factor needed to explode the star. Is this derivable analytically? | ||
+ | * How do trajectories differ when the factor is: half, equal, and twice the critical explosion value? | ||
+ | * Do all trajectories escape? | ||
+ | * Assume an initial composition for all fluid elements. | ||
+ | * How does the composition in each trajectory evolve? | ||
+ | * What does the final composition of the whole “star” look like? | ||
+ | * How does the final composition of the escaped trajectories compare to the total? | ||
+ | |||
+ | == Post-Processing nucleosynthesis == | ||
+ | |||
+ | * Extract a Lagrangian profile from the blast wave simulation and use the network to calculate the nucleosynthesis. | ||
+ | |||
+ | == Numerics of Blast Waves== | ||
+ | |||
+ | * Explore how resolution, dimensionality and the nature of the grid affect a blast wave simulation. | ||
+ | |||
+ | == Reaction Sensitivity studies == | ||
+ | |||
+ | * Change reactions in the network and examine the impact on the abundances. We can easily do this for CCSN, TNSN, novae, XRB, maybe others. | ||
+ | |||
+ | == Impact of Neutronization on supernova nucleosynthesis == | ||
+ | |||
+ | * Vary the initial electron fraction and examine how CCSN nucleosynthesis changes. | ||
+ | |||
+ | == hydro:== | ||
+ | |||
+ | * Simulate the effects of a near-earth supernova explosion at 10 pc | ||
+ | (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 supernova | ||
+ | explosion energy? Distance? Interstellar density? | ||
+ | |||
+ | |||
+ | == nuke network: == | ||
+ | |||
+ | * Simulate the s-process under AGB conditions. Compare to solar system | ||
+ | abundances and presolar grains. How does the result depend on initial | ||
+ | composition? How good is the waiting point approximation? | ||
+ | |||
+ | |||
+ | == BBN: == | ||
+ | |||
+ | * Quantify the sensitivities of the light elements to variations in the | ||
+ | key reaction rates. Propagate uncertainties in nuclear reation | ||
+ | rates via Monte Carlo to evaluate the uncertainties in the BBN predictions. | ||
+ | |||
+ | * Explore the consequences of new physics during BBN. This can include: adding | ||
+ | neutrino species, modificiation of the gravitational constant, and neutrino | ||
+ | degeneracy. For a more challenging calculation, consider the effect of | ||
+ | dark matter decays that dissociate 4He. For each of these, what is the | ||
+ | effect on the light elements? How can we use light element and cosmological | ||
+ | (e.g., CMB) observations to constrain these scenarios? | ||