How Li & Paczynski Model of Kilonova Fits GW170817 Optical Counterpart

Abstract

The original Li & Paczynski model of kilonova was compared with the observed bolometric optical light curve of the GW170817 electromagnetic counterpart. Perfect agreement is obtained for early observations up to 1.5 days since the time of merger.

7 pages, 1 figure, minor editorial changes, matches the published version

References in corpus (2)

• Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations
• Constraints on the ejecta of the GW170817 neutron-star merger from its electromagnetic emission

Cited by in corpus (1)

• Radioactive $\gamma$-Ray Emissions from Neutron Star Mergers