  Using hydrodynamic simulations of disc-galaxy major mergers, we investigate
the star formation history and remnant properties when various parametrizations
of a simple stellar feedback model are implemented. The simulations include
radiative cooling, a density-dependent star formation recipe and a model for
feedback from massive stars. The feedback model stores supernova feedback
energy within individual gas particles and dissipates this energy on a
time-scale specified by two free parameters; tau_fb, which sets the dissipative
time-scale, and n, which sets the effective equation of state in star-forming
regions. Using a self-consistent disc galaxy, modelled after a local Sbc
spiral, in both isolated and major-merger simulations, we investigate
parametrizations of the feedback model that are selected with respect to the
quiescent disc stability. These models produce a range of star formation
histories that are consistent with the star formation relation found by
Kennicutt. All major mergers produce a population of new stars that is highly
centrally concentrated, demonstrating a distinct break in the r1/4 surface
density profile, consistent with previous findings. The half-mass radius and
one-dimensional velocity dispersion are affected by the feedback model used.
Finally, we compare our results to those of previous simulations of star
formation in disc-galaxy major mergers, addressing the effects of star
formation normalization, the version of smoothed particle hydrodynamics (SPH)
employed and assumptions about the interstellar medium.
