PIRSA:21030026

Video URL

https://pirsa.org/21030026

The structure of Gamma Ray Bursts: beyond GRB 170817

Beniamini, P. (2021). The structure of Gamma Ray Bursts: beyond GRB 170817. Perimeter Institute for Theoretical Physics. https://pirsa.org/21030026

Beniamini, Paz. The structure of Gamma Ray Bursts: beyond GRB 170817. Perimeter Institute for Theoretical Physics, Mar. 11, 2021, https://pirsa.org/21030026 

          @misc{ scivideos_PIRSA:21030026,
            doi = {10.48660/21030026},
            url = {https://pirsa.org/21030026},
            author = {Beniamini, Paz},
            keywords = {Strong Gravity},
            language = {en},
            title = {The structure of Gamma Ray Bursts: beyond GRB 170817},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2021},
            month = {mar},
            note = {PIRSA:21030026 see, \url{https://scivideos.org/index.php/pirsa/21030026}}
          }

Paz Beniamini California Institute of Technology (Caltech)

Talk numberPIRSA:21030026
DOI10.48660/21030026
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

Combining information from the first gravitational wave detected gamma-ray burst, GRB 170817 with observations of cosmological GRBs holds important lessons for understanding the structure of GRB jets and the required conditions at the emitting region. It also re-frames our understanding of more commonly observed phenomena in GRBs, such as X-ray plateaus, and sets our expectations for future observations. I will present different lines of argument suggesting that efficient gamma-ray emission in GRBs has to be restricted to material with Lorentz factor > 50 and is most likely confined to a narrow region around the core. GRB jets viewed slightly beyond their jet cores, result in X-ray plateaus that are consistent with observed light-curves and naturally reproduce correlations between plateau and prompt emission properties. For jets viewed further off-axis (that are expected to be detected as future GW triggered events) we provide new analytical modelling that reveals two different types of light-curves that could be observed (single or double peaked) and outlines how the underlying physical properties can be recovered from such observations.