机构地区：[1]Shanghai Key Lab for Astrophysics,Shanghai Normal University,Shanghai 200234,China [2]School of Information Engineering,Guangzhou Panyu Polytechnic,Guangzhou 511483,China [3]Department of Physics,Zhejiang Normal University,Jinhua 321004,China [4]College of Mathematics and Physics,Guangxi Minzu University,Nanning 530006,China [5]Key Laboratory of Cosmology and Astrophysics(Liaoning),College of Sciences,Northeastern University,Shenyang 110819,China [6]Department of Physics,University of Rijeka,Rijeka 51000,Croatia [7]Center for Astrophysics,Guangzhou University,Guangzhou 510006,China [8]Key Laboratory for Astronomical Observation and Technology of Guangzhou,Guangzhou 510006,China [9]Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province,Guangzhou 510006,China
出 处：《Research in Astronomy and Astrophysics》2024年第6期156-169,共14页天文和天体物理学研究（英文版）
基 金：support from the National Natural Science Foundation of China(NSFC,Grant No.12203034);from the Shanghai Science and Technology Fund under grant No.22YF1431500;from the science research grants from the China Manned Space Project;support from the National Natural Science Foundation of China(NSFC,grant No.12203043);support from the National Natural Science Foundation of China(NSFC,grant No.11933002);support from the National Natural Science Foundation of China(NSFC,grant No.12173026);the National Key Research and Development Program of China(grant No.2022YFC2807303);the Shanghai Science and Technology Fund(grant No.23010503900);the Program for Professor of Special Appointment(Eastern Scholar)at Shanghai Institutions of Higher Learning;the Shuguang Program(23SG39)of the Shanghai Education Development Foundation and Shanghai Municipal Education Commission;support from the National Natural Science Foundation of China(NSFC,grant No.U2031201,and 11733001);the Scientific and Technological Cooperation Projects(20202023)between the People’s Republic of China and the Republic of Bulgaria;the science research grants from the China Manned Space Project with No.CMS-CSST-2021A06;partially supported by the Bulgarian National Science Fund of the Ministry of Education and Science under grants KP-06-H38/4(2019),KP-06-KITAJ/2(2020),and KP-06-H68/4(2022)。
摘 要：The location ofγ-ray emission of blazars remains a contested topic,inspiring the development of numerous investigative techniques to address this issue.In this work,we analyzed Fermiγ-ray light curves in the GeV and MeV bands,employing the discrete cross-correlation function method to discern time lags between the two bands.For 4C+21.35,Ton 599,B21420+32,and PKS 1510-089,we identified a time lag spanning several days,while for PKS 1441+25,the time lag was not statistically found.The results imply that the soft photons necessary for inverse Compton scattering predominantly originate from the dusty torus in the first four sources,whereas for PKS1441+25,they seem to be sourced mainly from the broad-line region.Further analysis of the opacity(τγγ)and the GeV spectra study supports the conclusion that the location of the dissipation region must be beyond the BLR to avoid significant absorption.Notably,for PKS 1441+25,the emission region is also posited to lie outside yet proximate to the BLR.The parameters of describing the emission region were obtained by fitting broadband spectral energy distribution with contemporaneous observation data.Our findings suggest that for the five TeV FSRQs,during Te V flaring events,the jet appears to maintain an equilibrium between the energy density of the magnetic field and that of the particles for all investigated sources,with the exceptions of 4C+21.35 and PKS1441+25.In terms of the overall jet power,particle energy is the dominant contributor,and the observed blazar radiation cannot be solely attributed to the magnetic field,except in the case of 4C+21.35.Consequently,magnetic reconnection is unlikely to be the primary mechanism behind particle acceleration in these systems.
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