Date:
Tue, 15/05/201812:30-13:30
Title: Lessons from GW170817 / GRB170817A
Abstract: The first detection of a gravitational wave signal from a binary neutron star merger, GW 170817, was also promptly accompanied by an electromagnetic counterpart in the form of a short duration gamma-ray burst, GRB 170817A. A huge global effort of multi-wavelength follow-up observations has led to the detection of kilonova emission in the optical, UV and NIR, as well as long-lived X-ray to radio afterglow emission. This unique event has a wide range of implications ranging from constraints on the neutron star equation of state and maximal mass, through the important role of such binary mergers in r-process nucleosynthesisin the universe, to the type of remnant that was produced, and the properties of the outflows that are produced in these mergers.In this talk I will focus on what can be learned from this event about the properties of the outflow that powered the prompt gamma-ray emission and the afterglow emission, and briefly outline the constraints on the type of compact remnant (black hole or massive neutron star) that was left in its aftermath.
Abstract: The first detection of a gravitational wave signal from a binary neutron star merger, GW 170817, was also promptly accompanied by an electromagnetic counterpart in the form of a short duration gamma-ray burst, GRB 170817A. A huge global effort of multi-wavelength follow-up observations has led to the detection of kilonova emission in the optical, UV and NIR, as well as long-lived X-ray to radio afterglow emission. This unique event has a wide range of implications ranging from constraints on the neutron star equation of state and maximal mass, through the important role of such binary mergers in r-process nucleosynthesisin the universe, to the type of remnant that was produced, and the properties of the outflows that are produced in these mergers.In this talk I will focus on what can be learned from this event about the properties of the outflow that powered the prompt gamma-ray emission and the afterglow emission, and briefly outline the constraints on the type of compact remnant (black hole or massive neutron star) that was left in its aftermath.