TY - JOUR
T1 - The coalescence rate of neutron star-white dwarf binaries
AU - Nyadzani, L.
AU - Razzaque, S.
N1 - Publisher Copyright:
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0).
PY - 2021/4/2
Y1 - 2021/4/2
N2 - When two compact objects such as black holes (BH), white dwarfs (WD), and neutron stars (NS) orbit a common centre of gravity, they emit energy in the form of gravitational waves (GW). The emission of GW will result in the two objects coalescing. In this work, we revisit the coalescence of NS-WD binary systems with the addition of one NS-WD binary system to the coalescing NS-WD binary systems sample. The addition of this new system increased the coalescence rate from previously estimated 4.11+−522556 Myr−1 to 8.0+−242.00 Myr−1 at the 90% confidence level.
AB - When two compact objects such as black holes (BH), white dwarfs (WD), and neutron stars (NS) orbit a common centre of gravity, they emit energy in the form of gravitational waves (GW). The emission of GW will result in the two objects coalescing. In this work, we revisit the coalescence of NS-WD binary systems with the addition of one NS-WD binary system to the coalescing NS-WD binary systems sample. The addition of this new system increased the coalescence rate from previously estimated 4.11+−522556 Myr−1 to 8.0+−242.00 Myr−1 at the 90% confidence level.
UR - http://www.scopus.com/inward/record.url?scp=85103899447&partnerID=8YFLogxK
M3 - Conference article
AN - SCOPUS:85103899447
SN - 1824-8039
VL - 371
JO - Proceedings of Science
JF - Proceedings of Science
T2 - 7th Annual Conference on High Energy Astrophysics in Southern Africa, HEASA 2019
Y2 - 28 August 2019 through 30 August 2019
ER -