首页|GRB 210610B:The Internal and External Plateau as Evidence for the Delayed Outflow of Magnetar

GRB 210610B:The Internal and External Plateau as Evidence for the Delayed Outflow of Magnetar

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After launching a jet,outflows of magnetar were used to account for the achromatic plateau of afterglow and the early X-ray flux plateau known as"internal plateau".The lack of detecting magnetic dipole emission together with the energy injection feature in a single observation poses confusion until the long gamma-ray burst(GRB)210610B is detected.GRB 210610B is presented with an optical bump following an early X-ray plateau during the afterglow phase.The plateau followed by a steep decline flux overlays in the steadily decaying X-ray flux with index αx,l～2.06,indicating an internal origin and that can be fitted by the spin-down luminosity law with the initial plateau luminosity log10Lx～48.29 erg s-1 and the characteristic spin-down timescale T～2818 s.A subsequent bump begins at～4000 s in the R band with a rising index αR,1～-0.30 and peaks at～14125 s,after which a decay index αR,2～0.87 and finally transiting to a steep decay with αR,3～1.77 achieve the closure relation of the external shock for the normal decay phase as well as the magnetar spin-down energy injection phase,provided that the average value of the photon index Γγ=1.80 derived from the spectral energy distributions(SEDs)between the X-ray and optical afterglow.The closure relation also works for the late X-ray flux.Akin to the traditional picture of GRB,the outflow powers the early X-ray plateau by dissipating energy internally and collides with the leading decelerating blast burst as time goes on,which could interpret the exotic feature of GRB 210610B.We carry out a Markov Chain Monte Carlo simulation and obtain a set of best parameters:εB(≌)4.7 × 10-5,εe(≌)0.15,EK,iso(≌)4.6 × 1053erg,T0(≌)832,A*(≌)0.10,Linj,0(≌)3.55 × 1050erg s-1.The artificial light curve can fit the afterglow data well.After that,we estimated the average Lorentz factor and the X-ray radiation efficiency of the later ejecta are 35％and 0.13％,respectively.

(stars:)gammaray burst:individual(GRB 210610B)(stars:)gammaray burst:generalstars:jets

韦逸宁、王祥高、林达斌、郑伟康、陈良军、闫圣钰、仪双喜、王琦、周子民、刘慧亚、梁恩维

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Guangxi Key Laboratory for Relativistic Astrophysics,School of Physical Science and Technology,Guangxi University,Nanning 530004,China

GXU-NAOC Center for Astrophysics and Space Sciences,Nanning 530004,China

Department of Astronomy,University of California,Berkeley,CA 94720-3411,USA

Department of Physics and Tsinghua Center for Astrophysics(THCA),Tsinghua University,Beijing 100084,China

School of Physics and Physical Engineering,Qufu Normal University,Qufu 273165,China

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National Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaProgramme of Bagui Scholars Programme(WXG)China Space Station Telescope(CSST)

12373042U19382011227300512133003

2024

10.1088/1674-4527/ad4d3a

天文和天体物理学研究
中国科学院国家天文台

天文和天体物理学研究

CSTPCD
影响因子：0.406
ISSN：1674-4527
年,卷(期)：2024.24(7)