Abstract
In these proceedings, we summarise the exploration so far of the relationship between the afterglow luminosity (measured at rest frame 200s; log L 200 s ) and average afterglow decay rate (measured from rest frame 200s onwards, α > 200 s ) of long duration Gamma-ray Bursts (GRBs), first reported in the optical/UV light curves of GRB afterglows. We show that this correlation is also present in the X-ray afterglows of GRBs as observed by Swift-XRT. We explore how the parameters of the correlation observed in both the X-ray and optical/UV light curves relate to each other and the prompt emission phase and whether these correlations are consistent with predictions of the standard afterglow model. We find that the observed correlations are consistent with a common underlying physical mechanism producing GRBs and their afterglows regardless of the detailed temporal behaviour. However, a basic afterglow model has difficulty explaining all the observed correlations. This leads us to briefly discuss alternative more complex models.
Highlights
Statistical investigations of large samples of Gamma-ray bursts (GRBs) aim to find common characteristics and correlations that link individual events and provide insight into the mechanisms common to Gamma-ray Bursts (GRBs)
For GRBs where the prompt emission contaminates the light curve, we re-computed the average decay index using only data beyond rest frame 200s that is not dominated by the steep decay and we exclude flaring episodes
Using a large sample of X-ray light curves, we find a correlation between log L200s and α>200s, which is in agreement with observations performed in the optical/UV using a smaller sample
Summary
Statistical investigations of large samples of Gamma-ray bursts (GRBs) aim to find common characteristics and correlations that link individual events and provide insight into the mechanisms common to GRBs. The luminosity distribution of GRB afterglow light curves is clustered and appears to be wider at early times and narrows as the afterglows fade. The luminosity distribution of GRB afterglow light curves is clustered and appears to be wider at early times and narrows as the afterglows fade This points towards the brightest GRB afterglows decaying more quickly than the less luminous afterglows. Galaxies 2017, 5, 4 we explored this hypothesis using a sample of optical/UV light curves. We tested for a correlation between logarithmic brightness (measured at rest frame 200s), log L200s and average decay rate of GRB afterglows (measured from rest frame 200s onwards), α>200s.
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
