Shan-Qin Wang

The Observer’s Guide to the Gamma-Ray Burst Supernova Connection

We present a detailed report of the connection between long-duration gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The discussion presented here places emphasis on how observations, and the modelling of observations, have constrained what we know about GRB-SNe. We discuss their photometric and spectroscopic properties, their role as cosmological probes, including their measured luminosity–decline relationships, and how they can be used to measure the Hubble constant. We present a statistical summary of their bolometric properties and use this to determine the properties of the “average” GRB-SN. We discuss their geometry and consider the various physical processes that are thought to power the luminosity of GRB-SNe and whether differences exist between GRB-SNe and the SNe associated with ultra-long-duration GRBs. We discuss how observations of their environments further constrain the physical properties of their progenitor stars and give a brief overview of the current theoretical paradigms of their central engines. We then present an overview of the radioactively powered transients that have been photometrically associated with short-duration GRBs, and we conclude by discussing what additional research is needed to further our understanding of GRB-SNe, in particular the role of binary-formation channels and the connection of GRB-SNe with superluminous SNe.

Superluminous Supernovae Powered by Magnetars: Late-time Light Curves and Hard Emission Leakage

Recently, researches performed by two groups have revealed that the magnetar spin-down energy injection model with full energy trapping can explain the early-time light curves of SN 2010gx, SN 2013dg, LSQ12dlf, SSS120810 and CSS121015, but fails to fit the late-time light curves of these Superluminous Supernovae (SLSNe). These results imply that the original magnetar-powered model is challenged in explaining these SLSNe. Our paper aims to simultaneously explain both the early- and late-time data/upper limits by considering the leakage of hard emissions. We incorporate quantitatively the leakage effect into the original magnetar-powered model and derive a new semi-analytical equation. Comparing the light curves reproduced by our revised magnetar-powered model to the observed data and/or upper limits of these five SLSNe, we found that the late-time light curves reproduced by our semi-analytical equation are in good agreement with the late-time observed data and/or upper limits of SN 2010gx, CSS121015, SN 2013dg and LSQ12dlf and the late-time excess of SSS120810, indicating that the magnetar-powered model might be responsible for these SLSNe and that the gamma ray and X-ray leakage are unavoidable when the hard photons were down-Comptonized to softer photons. To determine the details of the leakage effect and unveil the nature of SLSNe, more high quality bolometric light curves and spectra of SLSNe are required.

A Unified Energy-Reservoir Model Containing Contributions from 56 Ni and Neutron Stars and Its Implication to Luminous Type Ic Supernovae

Most type-Ic core-collapse supernovae (CCSNe) produce

Optical Transients Powered by Magnetars: Dynamics, Light Curves, and Transition to the Nebular Phase

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A Monte Carlo Approach to Magnetar-powered Transients: I. Hydrogen-deficient Superluminous Supernovae

Ni and neutron stars (NSs) or black holes (BHs). The dipole radiation of nascent NSs has usually been neglected in explaining supernovae (SNe) with peak absolute magnitude

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

M_{rm peak}

SOLVING THE 56Ni PUZZLE OF MAGNETAR-POWERED BROAD-LINED TYPE IC SUPERNOVAE

in any band are

A Monte Carlo approach to magnetar-powered transients: II. Broad-lined type Ic supernovae not associated with GRBs

gtrsim -19.5

A Multiple Ejecta-circumstellar Medium Interaction Model and Its Implications for Superluminous Supernovae iPTF15esb and iPTF13dcc

~mag, while the

Modeling The Most Luminous Supernova Associated with a Gamma-Ray Burst, SN 2011kl

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