Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9719w&link_type=abstract
American Astronomical Society, AAS Meeting #211, #97.19; Bulletin of the American Astronomical Society, Vol. 39, p.907
Astronomy and Astrophysics
Astronomy
Scientific paper
Galaxies are the most fundamental structures in the Universe. Their birth and evolution is driven by how they process their gas. The fuel for this evolution, gas, surrounds the Milky Way (MW) in a halo of hot, highly ionized, diffuse layers. Computer simulations have attempted to recreate these diffuse, extended layers of gas, but previous physical prescriptions have failed; the gas from stellar feedback cools too rapidly, falling to the center of the galaxy--the extended halo is not created. None have yet tried to compare observational data of the gaseous halo with their simulations. Serving as a representative of all spiral galaxies, the MW can be studied in great detail. Observational data of kinematics and ionization stages of the evolutionary fuel come from far ultra-violet spectral absorption lines; a bright light in the distant Universe (a quasar) illuminates a path through the halo to Earth, and the fingerprint of each layer of gas is imprinted at a specific location in the spectrum of light. We use a sophisticated Eulerian Gasdynamics and N-body simulation of the formation and evolution of the MW that includes detailed processing of the chemically enriched gas from stars. We replicate observational data in the simulations by creating synthetic spectra through the MW disk in all directions. I cover the entire sky in my code and then compare this with true observational sight lines observed by HST. This work seeks to duplicate HST results with the MW code by changing physical parameters, such as detailed processing of gas due to stellar feedback.
Ceverino Daniel
Churchill Chris
Klypin Anatoly
Widhalm Allison M.
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