1997/09/12 by Izumi Murakami, I. Murakami, Murakami, Izumi +2
Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Gamma-ray bursts and supernovae #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9709114
4 pages LaTeX, 3 PostScript figures, conf_iap.sty. To appear in the Proceedings of the 13th IAP Colloquium (July 1-5, 1997): Structure and Evolution of the IGM from QSO Absorption Line Systems
arxiv created 1997/09/12 · openalex publication_date 1997/09/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We have examined the metal enrichment of the intergalactic medium (IGM) based on a galactic wind model. A galactic wind driven by supernovae brings metallic gas to the IGM but not so far beyond the gravitational potential. The expanding velocity of the outflow depends on the star formation timescale. Examining 3D calculation for the IGM in CDM model, we find that only 10 % region has metallicity larger than 10-2Z\odot at z=3. Wide range of the IGM metallicity produces variety of CIV column densities for a fixed HI column density.