PIRSA:20110061

GRB Jets At All Angles

Ryan, G. (2020). GRB Jets At All Angles. Perimeter Institute. https://pirsa.org/20110061

Ryan, Geoffrey. GRB Jets At All Angles. Perimeter Institute, Nov. 26, 2020, https://pirsa.org/20110061 

          @misc{ pirsa_PIRSA:20110061,
            doi = {10.48660/20110061},
            url = {https://pirsa.org/20110061},
            author = {Ryan, Geoffrey},
            keywords = {Strong Gravity},
            language = {en},
            title = {GRB Jets At All Angles},
            publisher = {Perimeter Institute},
            year = {2020},
            month = {nov},
            note = {PIRSA:20110061 see, \url{https://pirsa.org}}
          }

Geoffrey Ryan

Perimeter Institute for Theoretical Physics

Talk number
PIRSA:20110061
Collection
Talk Type
Subject
Abstract

Abstract: Gamma-ray bursts (GRBs) associated with gravitational wave events are, and will likely continue to be, viewed at a much larger inclination than GRBs without gravitational wave detections.  Viewing GRBs and their afterglows at large inclination can massively affect the observed electromagnetic emission, as dramatically demonstrated by the binary neutron star merger event GW170817.  Analyzing this event and future ones requires an extension of the common GRB afterglow models which typically assume emission from a structureless (top-hat) jet viewed on-axis. I will review the evidence for inclination effects in GRB afterglows, and present a characterization of afterglows viewed at all angles from jets with and without structure. We find new closure relations for off-axis structured jets: the slope of the light curve is found in many cases to be a simple function of the inclination angle. With our theoretical tools in hand I will discuss new candidate kilonova events found in the GRB archive, showing features very similar to GW170817. Finally I will discuss our numerical model to calculate synthetic light curves and spectra, publicly available as the open source Python package afterglowpy, and the steps needed to improve our capabilities for the next LIGO observing run.