  We present, for the first time, numerical simulations of young tidal dwarf
galaxies (TDGs), including a self-consistent treatment of the tidal arm in
which they are embedded. Thereby, we do not rely on idealised initial
conditions, as the initial data of the presented simulation emerge from a
galaxy interaction simulation. By comparing models which are either embedded in
or isolated form the tidal arm, we demonstrate its importance on the evolution
of TDGs, as additional source of gas which can be accreted and is available for
subsequent conversion into stars. During the initial collapse of the proto-TDG,
with a duration of a few 100 Myr, the evolution of the embedded and isolated
TDGs are indistinguishable. Significant differences appear after the collapse
has halted and the further evolution is dominated by the possible accretion of
material form the surroundings of the TDGs. The inclusion of the tidal arm in
the simulation of TDGs results in roughly a doubling of the gas mass
($M_\mathrm{gas}$) and gas fraction ($f_\mathrm{gas}$), an increase in stellar
mass by a factor of 1.5 and a $\sim3$ times higher star formation rate (SFR)
compared to the isolated case. Moreover, we perform a parametric study on the
influence of different environmental effects, i.e. the tidal field and ram
pressure. Due to the orbit of the chosen initial conditions, no clear impact of
the environmental effects on the evolution of TDG candidates can be found.
