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Add to Calendar 12/11/2018 3:45 pm 12/11/2018 America/Chicago Astronomy Colloquium - "Electromagnetic counterparts to GW170817 and astrophysical implications" DESCRIPTION:
The neutron star merger GW170817 is the first gravitational-wave (GW) event
accompanied by electromagnetic radiation: prompt gamma-rays, uv/optical/IR kilonova, and broadband non-thermal afterglow. The signatures of kilonova in GW170817 are consistent with the picture that a substantial amount of material is ejected at merger and the ejecta is  composed of  r-process nuclei. In particular, the light curve from 0.5 to 70 days after the merger can be explained well with the radioactive power of r-process nuclei. I will discuss what we can learn from this observation about the composition of the ejecta and also discuss the nebular emission of kilonvoae. The second part of my talk, I will focus on the superluminal jet in GW170817 observed by VLBI. Using the afterglow light curve data and VLBI images, the jet's Lorentz factor, kinetic energy, and viewing angle are determined. I will discuss the implication of this jet  to short gamma-ray bursts and how these observations can improve the GW distance measurement, which leads to the improvement of the local Hubble constant measurement from the GW-only analysis.

 

\n\nSPEAKER:

Kenta Hotokezaka, Princeton University

134 Astronomy

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Astronomy Colloquium - "Electromagnetic counterparts to GW170817 and astrophysical implications"

Speaker Kenta Hotokezaka, Princeton University
Date: 12/11/2018
Time: 3:45 p.m.
Location:

134 Astronomy

Event Contact: Rebecca Bare
217-265-8226
rsbare@illinois.edu
Sponsor:

Astronomy Department

Event Type: Seminar/Symposium
 
The neutron star merger GW170817 is the first gravitational-wave (GW) event
accompanied by electromagnetic radiation: prompt gamma-rays, uv/optical/IR kilonova, and broadband non-thermal afterglow. The signatures of kilonova in GW170817 are consistent with the picture that a substantial amount of material is ejected at merger and the ejecta is  composed of  r-process nuclei. In particular, the light curve from 0.5 to 70 days after the merger can be explained well with the radioactive power of r-process nuclei. I will discuss what we can learn from this observation about the composition of the ejecta and also discuss the nebular emission of kilonvoae. The second part of my talk, I will focus on the superluminal jet in GW170817 observed by VLBI. Using the afterglow light curve data and VLBI images, the jet's Lorentz factor, kinetic energy, and viewing angle are determined. I will discuss the implication of this jet  to short gamma-ray bursts and how these observations can improve the GW distance measurement, which leads to the improvement of the local Hubble constant measurement from the GW-only analysis.

 

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