Gas Inflow and Outflow Histories in Disk Galaxies as Revealed from
  Observations of Distant Star-Forming Galaxies
  We investigate gas inflow and outflow histories in Milky Way-like disk
galaxies, to get new insights into the baryonic processes in galaxy formation
and evolution. For this purpose, we solve the equations for the evolutions of
the surface mass densities of gas and metals at each radius in a galactic disk,
based on the observed structural properties of distant star-forming galaxies,
including the redshift evolution of their stellar mass distribution, their
scaling relation between the mass of baryonic components, star formation rate
(SFR) and chemical abundance, as well as the supposed evolution of their radial
metallicity gradients (RMGs). We find that the efficiency of gas inflow for a
given SFR decreases with time and that the inflow rate is always nearly
proportional to the SFR. For gas outflow, although its efficiency for a given
SFR is a decreasing function of time, similarly to gas inflow, the outflow rate
is not necessarily proportional to the SFR and the relation between the outflow
rate and SFR strongly depends on the evolution of the adopted RMG. We also find
that the results on the outflow rate can be reproduced in the framework of
momentum-driven (energy-driven) wind mechanism if the RMG is steepening
(flattening) with time. Therefore if the well measured RMGs and their evolution
for Milky Way-like galaxies are obtained from future observations, then our
results will be useful to constrain the main driving mechanism for their
galactic outflows.
