Kilonova afterglow rate from spherical and axisymmetrical models

Detecting the afterglows of double-neutron star merger events is a challenging task because of the quick fading of the observed flux. In order to create an efficient observing strategy for their observing method, it is crucial to know their intrinsic rate. Unfortunately, the numerous models existing today predict this rate on a very wide range. Our goal in this paper is to compare the different levels of approximations in order to determine their reliability. We find that there is a significant discrepancy in the expected detection rate between the spherical and axisymmetrical models (similar to 18 and less than or similar to 1 yr(-1), respectively). In addition, choosing different models for the input parameters (for example, redshift and time delay distribution) has also a strong effect on the results.