impacting Earth in the foreseeable future is extremely small, it does not seem wise to reduce our chance of detecting such a threat by failing to process that survey data.

REFERENCES

Bate, M.R., and I.A. Bonnell. 2004. Computer simulations of star cluster formation via turbulent fragmentation. In The Formation and Evolution of Massive Young Star Clusters. H.J.G.L.M. Lamers, L.J. Smith, and A. Nota., eds., ASP Conference Series, 322. San Francisco, Calif.: Astronomical Society of the Pacific, p. 289.

Faucher-Giguere, C.-A., A. Lidz, and L. Hernquist. 2008. Numerical simulations unravel the cosmic web. Science 319:52.

Heitsch, F., M.-M. Mac Low, and R.S. Klessen. 2001. Gravitational collapse in turbulent molecular clouds II: MHD turbulence. The Astrophysical Journal 547: 280.

Krumholz, M.R., R.I. Klein, and C.F. McKee. 2007. Radiation-hydrodynamic simulations of collapse and fragmentation in massive protostellar cores. The Astrophysical Journal 656: 959.

Meakin, Casey A., and David Arnett. 2007. Turbulent convection in stellar interiors, I: Hydrodynamic simulation. The Astrophysical Journal 667 (1): 448-475.

NRC (National Research Council). 2001. Astronomy and Astrophysics in the New Millennium. Washington, D.C.: National Academy Press.

NRC. 2003. Connecting Quarks with the Cosmos: Eleven Science Questions for the New Century. Washington, D.C.: The National Academies Press.

NSTC (National Science and Technology Council). 2004. The Physics of the Universe: A Strategic Plan for Federal Research at the Intersection of Physics and Astronomy. Washington, D.C.: NSTC.

Springel, Volker, Simon D.M. White, Adrian Jenkins, et al. 2005. Simulations of the formation, evolution and clustering of galaxies and quasars, Nature 435: 629.



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