Quanlin Fan

Chinese Academy of Sciences

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Co-Authors

Xueshang Feng

Harbin Institute of Technology

Fengsi Wei

Harbin Institute of Technology

Changqing Xiang

Jishou University

Feng Xue-Shang

National Space Science Center

Chi Wang

National Space Science Center

Ya Xu

First Affiliated Hospital of Chongqing Medical University

Jian-shan Guo

National Space Science Center

Wei Feng-si

National Space Science Center

Changqing Xiang

Universiti Putra Malaysia

Lilin SUN

Cooperative Institutions

Chinese Academy of Sciences

National Space Science Center

Chinese Academy of Meteorological Sciences

University of Chinese Academy of Sciences

Harbin Institute of Technology

University of Science and Technology of China

Wuhan University

Changsha University of Science and Technology

Xi'an Jiaotong University

Purple Mountain Observatory

Author Statistics

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Numerical Simulation on a Possible Formation Mechanism of Interplanetary Magnetic Cloud Boundaries

Communications in Theoretical Physics (2003)

Quanlin Fan Wei Feng-si Feng Xue-Shang

The formation mechanism of the interplanetary magnetic cloud (MC) boundaries is numerically investigated by simulating the interactions between an MC of some initial momentum and a local interplanetary current sheet. The compressible 2.5D MHD equations are solved. Results show that the magnetic reconnection process is a possible formation mechanism when an MC interacts with a surrounding current sheet. A number of interesting features are found. For instance, the front boundary of the MCs is a magnetic reconnection boundary that could be caused by a driven reconnection ahead of the cloud, and the tail boundary might be caused by the driving of the entrained flow as a result of the Bernoulli principle. Analysis of the magnetic field and plasma data demonstrates that at these two boundaries appear large value of the plasma parameter β, clear increase of plasma temperature and density, distinct decrease of magnetic magnitude, and a transition of magnetic field direction of about 180 degrees. The outcome of the present simulation agrees qualitatively with the observational results on MC boundary inferred from IMP-8, etc.

Current sheet

Momentum (technical analysis)

Plasma sheet

10.1088/0253-6102/40/2/247

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Citations (4)

A Class of TVD Type Combined Numerical Scheme for MHD Equations with a Survey about Numerical Methods in Solar Wind Simulations

Springer eBooks (2003)

Xueshang Feng S. T. Wu Fengsi Wei Quanlin Fan

Total variation diminishing

Space Weather

10.1007/978-94-007-1069-6_5

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Citations (19)

Prediction tests by using ISF method for the geomagnetic disturbances

Science China Technological Sciences (2002)

Fengsi Wei Ya Xu Xueshang Feng Quanlin Fan

Space Weather

Geomagnetic secular variation

Ring current

Interplanetary scintillation

10.1360/02ye9060

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Citations (8)

A Possible Interpretation of Burst-Like Characteristics of Explosive Events

Communications in Theoretical Physics (2004)

Quanlin Fan Feng Xue-Shang Changqing Xiang

Explosive events have been observed to occur consecutively in bursts at intermittent locations along the boundary near the opposite polarity. The aim of the present paper is to explore a possible mechanism to interpret this burst-like characteristic of explosive events. The 2D magnetohydrodynamic (MHD) numerical simulations with resistivity have been carried out to reproduce the intermittent spatial-temporal magnetic reconnection events taking place along the long, compressible current sheet. The observed density enhancements in previously published results have been verified to be associated to magnetic reconnection sites. Late observational evidences, which support present attempts, have also been found, at least in morphological evolution of the consecutive explosive events.

Current sheet

Polarity (international relations)

10.1088/0253-6102/41/5/790

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Citations (2)

China’s Space Science Program (2025–2030): Strategic Priority Program on Space Science (III)

Chinese Journal of Space Science (2022)

Chi Wang Tingting SONG Peng SHI Ming Li Quanlin Fan

Space program

space science

10.11728/cjss2022.04.yg01

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Citations (7)

Magnetohydrodynamic simulations of turbulent magnetic reconnection

Physics of Plasmas (2004)

Quanlin Fan Xueshang Feng Changqing Xiang

Turbulent reconnection process in a one-dimensional current sheet is investigated by means of a two-dimensional compressible one-fluid magnetohydrodynamic simulation with spatially uniform, fixed resistivity. Turbulence is set up by adding to the sheet pinch small but finite level of broadband random-phased magnetic field components. To clarify the nonlinear spatial-temporal nature of the turbulent reconnection process the reconnection system is treated as an unforced initial value problem without any anomalous resistivity model adopted. Numerical results demonstrate the duality of turbulent reconnection, i.e., a transition from Sweet–Parker-like slow reconnection to Petschek-like fast reconnection in its nonlinear evolutionary process. The initial slow reconnection phase is characterized by many independent microreconnection events confined within the sheet region and a global reconnection rate mainly dependent on the initially added turbulence and insensitive to variations of the plasma β and resistivity. The formation and amplification of the major plasmoid leads the following reconnection process to a rapid reconnection stage with a fast reconnection rate of the order of 0.1 or even larger, drastically changing the topology of the global magnetic field. That is, the presence of magnetohydrodynamic turbulence in large-scale current sheets can raise the reconnection rate from small values on the order of the Sweet–Parker rate to high values on the order of the Petscheck rate through triggering an evolution toward fast magnetic reconnection. Meanwhile, the backward coupling between the small- and large-scale magnetic field dynamics has been properly represented through the present high resolution simulation. The undriven turbulent reconnection model established here expresses a solid numerical basis for the previous schematic two-step magnetic reconnection models and a possible explanation of two-stage energy release process of solar explosives.

Magnetohydrodynamic Turbulence

Current sheet

Plasmoid

10.1063/1.1806827

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Citations (12)

Numerical Simulation for the 16 August 1999 EUV Brightenings

Chinese Journal of Space Science (2008)

Xiaoming SHA Quanlin Fan

The 16 August 1999 EUV brightenings are numerically simulated by a third-order upwind compact scheme, basing on the TRACE observation. The present simulation can give a possible explanation to its formation and evolution. The numerical results show that the initial reconnection jets at around X-point are responsible for the occurrence of EUV brightening. The strong and superposed ejections caused by the first and second coalescence of magnetic islands are possibly related to the lifted material which initially appeared as absorption features and Later EUV-emitting structures respectively. The bi-directional reconnection jets may correspond to the lifted material that either continued to move upward along the apparently open field lines or fell down to the surface.

Extreme Ultraviolet Lithography

Coalescence (physics)

10.11728/cjss2008.06.507

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Citations (0)

Possible two-step solar energy release mechanism due to turbulent magnetic reconnection

Physics of Plasmas (2005)

Quanlin Fan Xueshang Feng Changqing Xiang

In this paper, a possible two-step solar magnetic energy release process attributed to turbulent magnetic reconnection is investigated by magnetohydrodynamic simulation for the purpose of accounting for the closely associated observational features including canceling magnetic features and different kinds of small-scale activities such as ultraviolet explosive events in the lower solar atmosphere. Numerical results based on realistic transition region physical parameters show that magnetic reconnections in a vertical turbulent current sheet consist of two stages, i.e., a first slow Sweet–Parker-like reconnection and a later rapid Petschek-like reconnection, where the latter fast reconnection phase seems a direct consequence of the initial slow reconnection phase when a critical state is reached. The formation of coherent plasmoid of various sizes and their coalescence play a central role in this complex nonlinear evolution. The “observed” values of the rate of cancellation flux as well as the approaching velocity of magnetic fragments of inverse polarity in present simulation are well consistent with the corresponding measurements in the latest observations. The difference between our turbulent magnetic reconnection two-step energy release model and other schematic two-step models is discussed and then possible application of present outcome to solar explosives is described.

Plasmoid

Solar flare

Current sheet

Nanoflares

Coalescence (physics)

10.1063/1.1862249

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Citations (1)

Simulation of small-scale coronal explosives due to magnetic reconnections

Physics of Plasmas (2003)

Quanlin Fan Xueshang Feng Changqing Xiang Dingkun Zhong

The dynamics of small-scale explosive phenomena in the lower corona have been simulated by solving the compressible magnetohydrodynamic equations. Numerical results show that the magnetic reconnections in a long coronal current sheet consist of a series of discrete small reconnection events, coalescence of magnetic islands, and plasmoid ejections, corresponding to the explosive events occurring intermittently and as bursts in a mentioned observational case. The generation of magnetic islands via multiple-X-point reconnection and their coalescence processes, to some extent, are qualitatively similar to the sequence of brightenings in the active region NOAA 8668. The strong ejections are possibly related to the recorded extreme ultraviolet (EUV) emitting structures. Morphological comparison and quantitative check of the plasma parameters support this candidate mechanism, and the idea that explosive events that appear to last long may not be single events, but a succession of explosive events either resolved or unresolved. The temporal energy conversion process is also examined.

Plasmoid

Coalescence (physics)

Extreme ultraviolet

Current sheet

Corona (planetary geology)

10.1063/1.1620999

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Citations (4)

Start-Time of Magnetic Reconnection in Interplanetary Space

Chinese Physics Letters (2003)

Quanlin Fan Wei Feng-si Feng Xue-Shang

Start-time of magnetic reconnection under typical interplanetary parameters has been numerically simulated by using the two-dimensional compressible magnetohydrodynamic equations with a third-order compact upwind scheme. Magnetic reconnection would occur near the interplanetary current sheet impacted by a plasmoid. Its initiation is associated with the interplanetary plasma parameter β and the momentum of the plasmoid. The higher the β value is, the faster the reconnection takes place. Meanwhile the reconnection occurs earlier with increasing the plasmoid momentum, and increasing driving velocity is more effective in initializing the reconnection than that of the plasma density when the other factors are kept to be the same. The evolution of the reconnection with the heliocentric distance is also investigated.

Plasmoid

Current sheet

Astrophysical plasma

Momentum (technical analysis)

10.1088/0256-307x/20/4/328

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Citations (1)