The Statistics Of Short GRB Afterglows And Shock Breakout Of A Mergernova

The discovery of gravitational-wave signal(GW 170817)from the coalescing bi-nary neutron stars by the LIGO,marks the beginning of the era of multi-messenger astronomy.As the brightest electromagnetic counterpart of gravitational wave event from binary neutron stars,short gamma-ray bursts play an important role in the i-dentification and localization of source of gravitational-wave.Unlike long gamma-ray bursts,which come from the collapse of massive stars,short gamma-ray bursts are generally thought to come from the merger of two compact stars(neutron stars-neu-tron stars,or neutron stars-black holes).The consistency between GW 170817 and GRB 170817A strongly supports the above view.Merger of binary neutron stars pro-duce an extremely relativistic jet in the axial direction,resulting in a short gamma-ray burst.Generally,after the merger,a black hole will form at center.However,some of the radiation signatures were founded in the afterglow of the short gamma-ray bursts indicating sustained energy activity in the center.Thus,the merger of binary neutron stars is more likely to produce a massive neutron star(or magnetar)as a remnant.Neutron st,ars can power a gamma-ray burst flows over a long period of time,so t,hey can form plateau of the afterglow or flare.At the same time,because of the injection of energy from a neutron star,the so-called mergernova radiation is also formed.As one of electromagnetic counterparts of gravitational wave signal,the mergernova is very helpful to confirm of gravitational wave signal in off-axis observation.Based on the importance of afterglow of short gamma-ray bursts and mergernova,this paper focuses on these two aspects.The first chapter gives the introduction of some basic knowledge and research status.The second chapter shows the statistical analysis of X-ray and optical afterglow observation data of short gamma-ray bursts.By collecting and organizing relevant data and mathematical fitting,it provides data basis for further classification and model int,erpretation.The third chapter discusses a comprehensive theoretical analysis and fitting of a special transient source GRB 130603B.The results show that the energy injection from the central neutron star can more consistently explain the multi-band observations of GRB 130603B.The last chapter is the summary and prospect.