Numerical simulations of outflows in quasars: the microphysics of BAL winds

Details Numerical simulations of outflows in quasars: the microphysics of BAL winds Numerical simulations of outflows in quasars: the microphysics of BAL winds

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9922f&link_type=abstract

HST Proposal ID #9922

Physics

Hst Proposal Id #9922 Agn/Quasars

Scientific paper

Mass outflow from Broad Absorption Line {BAL} quasars is best studied with resonant absorption lines that occur across the UV. Analysis of the lines reveals the chemical composition, energetics, and acceleration of the ejected material, and offers clues to the physics of the central powerhouse. HST has allowed this phenomenon to be studied in great detail. HST spectra are analyzed by reference to large scale plasma simulations which take into account the detailed microphysics of the gas. However, the presence of such a fast flow changes some of the assumptions that are the basis of current plasma codes ? in particular the assumption that the gas is in a local steady state. Actually, the flow introduces advection terms into all the rate equations, its energetics can affect the thermal balance of the gas, and high velocities affects the line and continuum transfer. This proposal requests support for the enhancement of the spectral simulation code Cloudy to make it fully appropriate for BAL outflows. The specific problems to be addressed are the radiative transport of lines and continua, which become complicated for such high- speed flows. I will also create grids of predictions that span the range of parameters seen in BAL quasars, but which include the effects of the outflow on both the physical state of the gas and its resulting spectrum.

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