  The theory of inflation is one of the fundamental and revolutionary
developments of modern cosmology that became able to explain many issues of
early universe in the context of the standard cosmological model (SCM).
However, the initial singularity of the universe, where physics is indefinite,
is still obscure in the combined `SCM+inflation' scenario. An alternative to
`SCM+inflation' without the initial singularity is thus always welcome, and
bouncing cosmology is an attempt of that. The current work is thus motivated to
investigate the bouncing solutions in modified gravity theories when the
background universe is described by the spatially flat
Friedmann-Lemaitre-Robertson-Walker (FLRW) geometry. We show that the simplest
way to obtain the bouncing cosmologies in such spacetime is to consider some
kind of Lagrangians whose gravitational sector depends only on the square of
the Hubble parameter of the FLRW universe. For these modified Lagrangians, the
corresponding Friedmann equation, a constraint in the dynamics of the universe,
depicts a curve in the phase space $(H,rho)$, where $H$ is the Hubble parameter
and $rho$ being the energy density of the universe. As a consequence, a
bouncing cosmology is obtained when this curve is closed and crosses the axis
$H = 0$ at least twice, and whose simplest particular example is the ellipse
depicting the well-known holonomy corrected Friedmann equation in Loop Quantum
Cosmology (LQC). Sometimes, a crucial point in such theories is the appearance
of the Ostrogradski instability at the perturbative level, however, fortunately
enough, in the present work as long as the linear level of perturbations is
concerned, this instability does not appear but such instability may appear at
the higher-order of perturbations.
