  The gas distribution in galaxies is smooth on large scales but is usually
inhomogeneous as well as time-dependent on smaller scales. The time-dependence
originates from processes such as cloud formation, their collisions and
supernovae (SNe) explosions. The inhomogeneities in the matter distribution
give rise to variations in the local galactic gravitational potential, which
can contribute towards dynamically coupling the gas disk to the stellar and the
dark matter (DM) components of the galaxy. Specifically, multiple supernovae
occurring in young stellar clusters give rise to superbubbles (SB), which
modify the local acceleration field and alter the energy and momentum of stars
of DM particles traversing them, in broad analogy to the dynamical friction
caused by a massive object. We aim to quantify how the acceleration field from
SBs causes dynamical friction and contributes to the secular evolution of
galaxies. In order to assess this, we construct the density modifications to
the gas distribution that mimics a SB. By evaluating the acceleration field
from these density modifications, we see how the momentum or angular momentum
of the gas hosting the SBs changes when stars pass through the SB. Combining
the effects of all the stars and SBs we, construct an empirical approximation
formula for the momentum loss in homogeneous and isotropic cases. We find that
the rate at which the gas disc loses its specific angular momentum via the
above process is up to 4% per Gyr, which translates to under half of its
original value over the lifetime of the disc. Finally, we studied how the
dynamical coupling of the gas disk with the DM halo depends on assumptions on
the halo kinematics (e.g. rotation) and found a ~0.3% variation in the gas disc
secular evolution between different DM kinematic models.
