An Ellerman Bomb(EB)is a kind of small scale reconnection event,which is ubiquitously formed in the upper photosphere or the lower chromosphere.The low temperature(<10,000 K)and high density(~1019–1022)plasma ther...An Ellerman Bomb(EB)is a kind of small scale reconnection event,which is ubiquitously formed in the upper photosphere or the lower chromosphere.The low temperature(<10,000 K)and high density(~1019–1022)plasma there makes the magnetic reconnection process strongly influenced by partially ionized effects and radiative cooling.This work studies the highβmagnetic reconnection near the solar temperature minimum region based on high-resolution 2.5D magnetohydrodynamics simulations.The time-dependent ionization degree of hydrogen and helium are included to realize more realistic diffusivities,viscosity and radiative cooling in simulations.Numerical results show that the reconnection rate is smaller than 0.01 and decreases with time during the early quasi-steady stage,then sharply increases to a value above 0.05 in the later stage as the plasmoid instability takes place.Both the large value ofηen(magnetic diffusion caused by the electron-neutral collision)and the plasmoid instability contribute to the fast magnetic reconnection in the EB-like event.The interactions and coalescence of plasmoids strongly enhance the local compression heating effect,which becomes the dominant mechanism for heating in EBs after plasmoid instability appears.However,the Joule heating contributed byηen can play a major role to heat plasmas when the magnetic reconnection in EBs is during the quasi-steady stage with smaller temperature increases.The results also show that the radiative cooling effect suppresses the temperature increase to a reasonable range,and increases the reconnection rate and generation of thermal energy.展开更多
Ellerman bombs(EBs)and ultraviolet(UV)bursts are common brightening phenomena,which are usually generated in the low solar atmosphere of emerging flux regions.In this paper,we have investigated the emergence of an ini...Ellerman bombs(EBs)and ultraviolet(UV)bursts are common brightening phenomena,which are usually generated in the low solar atmosphere of emerging flux regions.In this paper,we have investigated the emergence of an initial un-twisted magnetic flux rope based on three-dimensional(3 D)magneto-hydrodynamic(MHD)simulations.The EB-like and UV burst-like activities successively appear in the U-shaped part of the undulating magnetic fields triggered by the Parker instability.The EB-like activity starts to appear earlier and lasts for about 80 seconds.Six minutes later,a much hotter UV burstlike event starts to appear and lasts for about 60 seconds.Along the direction vertical to the solar surface,both the EB and UV burst start in the low chromosphere,but the UV burst extends to a higher altitude in the up chromosphere.The regions with apparent temperature increase in the EB and UV burst are both located inside the small twisted flux ropes generated in magnetic reconnection processes,which are consistent with the previous 2 D simulations that most hot regions are usually located inside the magnetic islands.However,the twisted flux rope corresponding to the EB is only strongly heated after it floats up to an altitude much higher than the reconnection site during that period.Our analyses show that the EB is heated by the shocks driven by the strong horizontal flows at two sides of the U-shaped magnetic fields.The twisted flux rope corresponding to the UV burst is heated by the driven magnetic reconnection process.展开更多
基金supported by the National Key R&D Program of China No.2022YFF0503800the National Natural Science Foundation of China(NSFC,Grant Nos.11973083 and 11933009)+6 种基金the Strategic Priority Research Program of CAS with grants XDA17040507the outstanding member of the Youth Innovation Promotion Association CAS(No.Y2021024)the Applied Basic Research of Yunnan Province in China Grant 2018FB009the Yunling Talent Project for the Youththe project of the Group for Innovation of Yunnan Province grant 2018HC023the Yunling Scholar Project of the Yunnan Province and the Yunnan Province Scientist Workshop of Solar PhysicsYunnan Key Laboratory of Solar Physics and Space Exploration(No.202205AG070009)。
文摘An Ellerman Bomb(EB)is a kind of small scale reconnection event,which is ubiquitously formed in the upper photosphere or the lower chromosphere.The low temperature(<10,000 K)and high density(~1019–1022)plasma there makes the magnetic reconnection process strongly influenced by partially ionized effects and radiative cooling.This work studies the highβmagnetic reconnection near the solar temperature minimum region based on high-resolution 2.5D magnetohydrodynamics simulations.The time-dependent ionization degree of hydrogen and helium are included to realize more realistic diffusivities,viscosity and radiative cooling in simulations.Numerical results show that the reconnection rate is smaller than 0.01 and decreases with time during the early quasi-steady stage,then sharply increases to a value above 0.05 in the later stage as the plasmoid instability takes place.Both the large value ofηen(magnetic diffusion caused by the electron-neutral collision)and the plasmoid instability contribute to the fast magnetic reconnection in the EB-like event.The interactions and coalescence of plasmoids strongly enhance the local compression heating effect,which becomes the dominant mechanism for heating in EBs after plasmoid instability appears.However,the Joule heating contributed byηen can play a major role to heat plasmas when the magnetic reconnection in EBs is during the quasi-steady stage with smaller temperature increases.The results also show that the radiative cooling effect suppresses the temperature increase to a reasonable range,and increases the reconnection rate and generation of thermal energy.
基金supported by the National Natural Science Foundation of China(NSFC,Grant Nos.11973083 and 11933009)the Strategic Priority Research Program of CAS(Grant Nos.XDA17040507 and QYZDJ-SSWSLH012)+7 种基金the grants associated with the Yunling Scholar Project of the Yunnan Province and the Yunnan Province Scientist Workshop of Solar Physicsthe Youth Innovation Promotion Association CAS 2017the Applied Basic Research of Yunnan Province in China(Grant 2018FB009)the Yunnan Ten-Thousand Talents Plan-Young top talentsthe project of the Group for Innovation of Yunnan Province(Grant 2018HC023)the Yunnan Ten-Thousand Talents Plan-Yunling Scholar Projectthe Special Program for Applied Research on Super Computation of the NSFC-Guangdong Joint Fund(NSFC015-460,NSFC2015-463,the second phase)Computational Solar Physics Laboratory of Yunnan Observatories,the key Laboratory of Solar Activity(Grant KLSA202103)。
文摘Ellerman bombs(EBs)and ultraviolet(UV)bursts are common brightening phenomena,which are usually generated in the low solar atmosphere of emerging flux regions.In this paper,we have investigated the emergence of an initial un-twisted magnetic flux rope based on three-dimensional(3 D)magneto-hydrodynamic(MHD)simulations.The EB-like and UV burst-like activities successively appear in the U-shaped part of the undulating magnetic fields triggered by the Parker instability.The EB-like activity starts to appear earlier and lasts for about 80 seconds.Six minutes later,a much hotter UV burstlike event starts to appear and lasts for about 60 seconds.Along the direction vertical to the solar surface,both the EB and UV burst start in the low chromosphere,but the UV burst extends to a higher altitude in the up chromosphere.The regions with apparent temperature increase in the EB and UV burst are both located inside the small twisted flux ropes generated in magnetic reconnection processes,which are consistent with the previous 2 D simulations that most hot regions are usually located inside the magnetic islands.However,the twisted flux rope corresponding to the EB is only strongly heated after it floats up to an altitude much higher than the reconnection site during that period.Our analyses show that the EB is heated by the shocks driven by the strong horizontal flows at two sides of the U-shaped magnetic fields.The twisted flux rope corresponding to the UV burst is heated by the driven magnetic reconnection process.
