Studies On The Physical Properties Of Supernovae Associated With Gamma-Ray Bursts

Core collapse supernovae（SNe）originating from the deaths of massive stars and Gamma-ray bursts（GRBs）originating from the deaths of massive stars or the mergers of compact stars are the extreme high-energy explosion phenomena,and important objects of research of high-energy astrophysics and time-domain astronomy.Studying SNe associated with GRBs（GRB-SNe）would help understand the progenitors,the circumburst medium,as well as the central engines of GRBs.To date,there are about 60 GRBs-SNe having been discovered,observed,and confirmed.This thesis briefly reviews the observational properties and theoretical scenarios of GRBs and SNe（the first chapter）,and study the physical properties of four typical GRB-SNe（the second and third chapters）.In the second chapter,we select three GRB-SNe（GRB 011121/SN 2011ke,GRB 130702A/SN 2013dx,and GRB 161219B/SN 2016jca）that have ample observational data to constitute a sample studied.We assume that the spectral energy distributions（SEDs）of the GRB-SNe are UV-absorbing blackbody ones,and directly fit their multi-band light curves to get their physical properties,which are the ejecta mass,the ejecta velocity,the ⁵⁶Ni mass,the kinetic energy,and so on.Considering the fact that the flux of the SNe is mixed with the flux from the GRB afterglows,we use the broken power-law afterglow plus ⁵⁶Ni model to fit their multi-band light curves.The fits shows that the ⁵⁶Ni masses are about 1.5times that of the corresponding values in the literature,and that the peak luminosities of the bolometric light curves calculated from the fits are about 2times those of the bolometric light curves constructed in the literature.In the third chapter,we adopt the cooling plus ⁵⁶Ni and the afterglow plus cooling plus ⁵⁶Ni model to fit the multi-band light curves of GRB 100316D/SN2010bh,getting its physical parameters and finding that the ⁵⁶Ni mass and the peak bolometric luminosity of SN 2010bh are about 2.2 and 2.7 times those in the literature,respectively.The results indicate the previous researchers underestimate the bolometric luminosities of GRB-SNe,and underestimate the ⁵⁶Ni masses when they fit the bolometric light curves.This is because they omit the flux in ultraviolet（UV）and/or infrared（IR）bands in the process of constructing the bolometric light curves.Our method can avoid underestimating the bolometric luminosities and⁵⁶Ni masses.Especially,our method can be used for some GRB-SNe that have observations in only few bands in same epochs or even in the whole evolution.The fourth chapter outlooks the research prospects in the field of GRB-SNe.