  Simulations of idealised star-forming filaments of finite length typically
show core growth which is dominated by two cores forming at its respective end.
The end cores form due to a strong increasing acceleration at the filament ends
which leads to a sweep-up of material during the filament collapse along its
axis. As this growth mode is typically faster than any other core formation
mode in a filament, the end cores usually dominate in mass and density compared
to other cores forming inside a filament. However, observations of star-forming
filaments do not show this prevalence of cores at the filament ends. We explore
a possible mechanism to slow the growth of the end cores using numerical
simulations of simultaneous filament and embedded core formation, in our case a
radially accreting filament forming in a finite converging flow. While such a
setup still leads to end cores, they soon begin to move inwards and a density
gradient is formed outside of the cores by the continued accumulation of
material. As a result, the outermost cores are not longer located at the exact
ends of the filament and the density gradient softens the inward gravitational
acceleration of the cores. Therefore, the two end cores do not grow as fast as
expected and thus do not dominate over other core formation modes in the
filament.
