This webpage allows to compute kilonovae properties for BNS mergers. Formulas are implemented following Class.Quant.Grav. 34 (2017) no.10, 105014. The implementation is done by Kyohei Kawaguchi and Tim Dietrich and is based on the kilonovae lightcurve generator for black hole-neutron star systems of Kyohei Kawaguchi. For questions please contact us.

The ejecta fits (left side) are obtained from a large number on numerical relativity simulations, see Tab. 1 of
Class.Quant.Grav. 34 (2017) no.10, 105014 for more details.
The lightcurves can be computed from the ejecta estimates obtained by the fitting formulas or user specified values.
The lightcurves are based on a simplified analytical model, which makes use of bolometric corrections computed from the
Monte-Carlo simulations of
Masaomi Tanaka.
For the bolometric corrections the numerical results (click * Use Tabulated Bolometric Corrections*) or analytic representation can be used.

* 3D rendering of the ejecta from a BNS merger *

Ejecta mass M_{ej}[M_{sun}] |
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Averaged ejecta velocity v_{ej}[c] |
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Minimum ejecta velocity v_{min}[c] |
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Latitudinal openning angle θ_{ej}[rad.] |
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Longitudinal openning angle ϕ_{ej}[rad.] |
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Opacity κ[cm^{2}/g] |
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Heating rate coefficient ϵ_{0}[erg/g/s] |
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Heating rate power α | : |

Thermalization efficiency ϵ_{th} |
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Duration [days] | : |

Use Tabulated Bolometric Correction | : |

NS Mass 1 M_{1}[M_{sun}] |
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NS bayron mass 1 M_{1,*}[M_{sun}] |
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NS Compactness 1 C_{1} |
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NS Mass 2 M_{2}[M_{sun}] |
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NS bayron mass 2 M_{2,*}[M_{sun}] |
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NS Compactness 2 C_{1} |
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M_{ej}= 0. M_{sun}

v_{ej}= 0. c

θ_{ej}=0. [rad.]

ϕ_{ej}=0. [rad.]

v

θ

ϕ