Study On The Evolution And Optical Variability Of Blazars

Blazar is a special subclass of the active galaxy nucleus and plays a very important role in the study of galaxy physics.It has a strong relativistic bunching effect,so it exhibits high luminosity,high polarization,fast and large optical change,jet Point to extreme physical properties such as the observer.Evolution and light change are two important observation phenomena of the flare variant,which reflects that the internal structure,activity process and nature of the flare variant are very complicated.Therefore,our research on evolutionary sequences and light change phenomena helps to further understand the flares and active galaxy nuclei,and the launch of Fermi satellites has enabled us to obtain more observation data and enable us to obtain more astronomical objects of this type.More physical information,so it is also important to study the evolutionary sequence and photoperiod of the Fermi variant.The first chapter of this article will first introduce the basic characteristics,classification,and models of active galaxy nuclei,as well as the observational characteristics and energy spectrum characteristics of Fermi variants.The second chapter mainly introduces the synchrotron radiation,inverse Compton scattering and the radiation model of the glare variant in detail.The third chapter introduces the light change time scale,classification and light change model of the flares.And we collected and calculated 734 samples of Fermi blazars in Chapter 4.the sample included 322 BL Lac objects and 412 flat spectrum radio quasars?FSRQs?.Then the distribution of redshift,black hole mass and gamma ray luminosity of each subclass were researched,and the relationships between redshift,BH mass and gamma ray luminosity were discussed.The results are as follows:1)According to the redshift and gamma ray luminosity from high to low,the evolution sequence of Fermi blazars follows:FSRQs?BL Lacs,and HSPs?ISPs?LSPs,but the evolution sequence obtained from high to low black hole mass is different.This may be due to the estimation error of the black hole mass and the small number of black hole mass samples;2)there is a significant positive correlation between the redshift and black hole mass,between black hole mass and gamma ray luminosity of each subclass of Fermi blazars;3)There is a significant inverse correlation between either the red shift or the gamma ray luminosity and the synchronous peak frequency of each subclass of Fermi blazars,there is no correlation between black hole mass and synchronous peak frequency.In Chapter 5,the 15 GHz optical variable data of the sources BL Lac PKS J2134-0153 and FSRQ PKS J0805-0111 published by the Owens Valley Observatory were studied for the optical variable period.Two sources were obtained using the LSP and WWZ methods.We have found that there is a light change period of 4.68±0.73years in BL Lac PKS J2134-0153 and a light change period of 3.38±0.4 years in FSRQ J0805-0111.These two periods have high confidence.?>5?,and use the false alarm probability and Monte Carlo simulation methods to test the significance of the obtained period.The confidence level of the period is considered to be greater than 5?.Spiral jets,thermal instability of the accretion disk,and supermassive black hole model interprets the obtained light variable period,and finally considers it to be a supermassive black hole system,and calculates the distance between the main black hole and the secondary black hole in the double black hole system are 1.83×10¹⁶cm and 1.43×10¹⁶cm.Finally,according to the obtained optical variable period,the next time when the two sources reach the peak value of traffic are predicted respectively.