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Kilonova afterglow rate from spherical and axisymmetrical models
Author(s) -
Kóbori J.
Publication year - 2019
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201913660
Subject(s) - afterglow , redshift , neutron star , physics , flux (metallurgy) , range (aeronautics) , reliability (semiconductor) , kilonova , astrophysics , fading , computational physics , gamma ray burst , statistical physics , computer science , algorithm , ligo , gravitational wave , aerospace engineering , quantum mechanics , materials science , galaxy , power (physics) , decoding methods , engineering , metallurgy
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 ( ∼18 and ≲ 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.