THE ROLES OF RADIATION AND RAM PRESSURE IN DRIVING GALACTIC WINDS

We study gaseous outflows from disk galaxies driven by the combined effects of ram pressure on cold gas clouds and radiation pressure on dust grains. Taking into account the gravity due to disk, bulge, and dark matter halo, and assuming continuous star formation in the disk, we show that radiation or ram pressure alone is not sufficient to drive escaping winds from disk galaxies and that both processes contribute. We show that in the parameter space of star formation rate (SFR) and rotation speed of galaxies the wind speed in galaxies with rotation speeds v(c) <= 200 km s(-1) and SFR <= 100 M-circle dot yr(-1) has a larger contribution from ram pressure, and that in high-mass galaxies with large SFR radiation from the disk has a greater role in driving galactic winds. The ratio of wind speed to circular speed can be approximated as v(w)/v(c) similar to 10(0.7) [SFR/50 M-circle dot yr(-1)](0.4) [v(c)/120 km s(-1)](-1.25). We show that this conclusion is borne out by observations of galactic winds at low and high redshift and also of circumgalactic gas. We also estimate the mass loading factors under the combined effect of ram and radiation pressure, and show that the ratio of mass-loss rate to SFR scales roughly as v(c)(-1) Sigma(-1)(g), where Sigma(g) is the gas column density in the disk.