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3D Outflows from Population III Stars: A Hydrodynamic Simulation Study

Explore the dynamics of outflows from massive, zero-metallicity Population III stars using 3D hydro simulations. Investigate angular momentum transport, outflow trajectories, neutrino emission, nucleosynthesis, and more. Gain insights into the properties of gamma-ray burst ejecta.

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3D Outflows from Population III Stars: A Hydrodynamic Simulation Study

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  1. GRB Outflows from Pop III Stars Aimee Hungerford, Gabe Rockefeller Chris Fryer, Patrick Young Los Alamos National Laboratory

  2. Motivation • Collapsar model is the favored mechanism for long duration GRBs • Pop III stars naturally satisfy the key ingredients needed for the collapsar model • Massive star • Low Metallicity • 3D Hydro simulations of these objects can provide insight into the properties of GRB ejecta.

  3. Outline • Hydro Simulations • Flows don’t really show a disk • Angular momentum transport • Outflow trajectories • Neutrino Emission • Average energy and luminosity • Ye evolution • Preliminary Nucleosynthesis

  4. Model(up to t = 5 sec) • 60 Msun (Hydrogen envelope present) • Zero Metallicity • Fast Rotating (B braking neglected) • Accretion Rate (roughly 0.1 Msuns-1) • MBH = ~2 Msun • boundary at R = 10 km • Newtonian gravity • 11 x 1051 erg explosion

  5. Outflows Spiral density wave pattern seen face-on. Convective-like flows are evident in edge-on view…not very “disk-like” at all.

  6. Angular Momentum Transport Angular momentum is being transported inward (red) and outward (blue) suggesting very different flow dynamics than those in a typical alpha disk model.

  7. Outflow Trajectory Sample trajectories from our 3D collapsar model and a disk wind model (Pruet, Thompson & Hoffman 2004) for comparison.

  8. Neutrino Fluxes • Electron fraction is reset by neutrinos, but does not achieve the equilibrium (ye near 0.5) implied by luminosity and mean energy of and .

  9. Nucleosynthesis

  10. Conclusions • 3D engine structure seems to be more complicated than expected. • Very energetic explosion is launched (even without a jet component.) • Electron fraction is uncertain and sets the nucleosynthesis of the outflow material. • “classical” r-process synthesis seems unlikely.

  11. Set-up and Simulation Zero metallicity star 2.5 million particles for inner 5 solar masses ~100,000-200,000 cpu hours per run Note High Angular Momentum (with respect to the angular momentum of the innermost stable circular orbit) in the first 2 solar masses Collapse - 60 Solar Mass Progenitor

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