Jinbin Cao

Beihang University

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Co-Authors

H. S. Fu

Beihang University

L. Y. Li

Beihang University

Haoyu Lu

Ministry of Industry and Information Technology

I. Dandouras

Institut de Recherche en Astrophysique et Planétologie

H. Rème

Centre National de la Recherche Scientifique

Yiqun Yu

Beihang University

Jiang Yu

Sun Yat-sen University

Z. Wang

Beihang University

Jun Cui

Sun Yat-sen University

Wenlong Liu

Beihang University

Cooperative Institutions

Chinese Academy of Sciences

282

Beihang University

168

National Space Science Center

158

University of Chinese Academy of Sciences

122

Ministry of Industry and Information Technology

University of Science and Technology of China

Centre National de la Recherche Scientifique

University of California, Los Angeles

Peking University

Institute of Geology and Geophysics

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Autogenous Electron Acceleration by Ion Flow Vortex in Space Plasmas

The Astrophysical Journal (2025)

C. M. Liu Jinbin Cao Y. Y. Liu E. A. Kronberg X. N. Xing

Abstract Plasma flow vortexes are ubiquitous in space and astrophysical settings and play a vital role in energy and mass transport, contributing to formation of stars and planets, launching and dissipation of astrophysical jets, and coupling between planetary magnetospheres and ionospheres. Here we present in situ observations showing that energetic electrons with energies up to 250 keV can be directly generated inside an ion flow vortex with finite spatial scale. The electron acceleration is achieved by establishment of Fermi acceleration trap and parallel electrostatic potential within the flow vortex, leading to dramatic enhancement of energetic electron flux by at least 1 order of magnitude. The accelerated electrons can drive mass and energy transport along local magnetic field lines and serve as a free energy source for broadband electrostatic emissions. Our observations, suggesting that the ion flow vortex can serve as novel electron accelerators, can be fundamentally important for understanding energetic phenomena in the cosmos, such as nonthermal emissions near astrophysical jets and killer electrons in geospace.

Astrophysical plasma

10.3847/1538-4357/ada269

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Estimating the corotation lag of the plasmasphere based on the electric field measurements of the Van Allen Probes

Advances in Space Research (2023)

Ziqi Zhang Wenlong Liu Dianjun Zhang Jinbin Cao

Plasmasphere

Van Allen Probes

Rotation period

10.1016/j.asr.2023.10.022

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Citations (0)

In-flight observations of electromagnetic interferences emitted by satellite

Science China Technological Sciences (2009)

Jinbin Cao Junying Yang ShiGan Yuan Xuhui Shen YuanMo Liu

Electromagnetic spectrum

10.1007/s11431-009-0101-9

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Citations (7)

Statistical Correlation Analysis of Field‐Aligned Currents Measured by Swarm

Journal of Geophysical Research Space Physics (2018)

Junying Yang M. W. Dunlop H. Lühr Chao Xiong Yanyan Yang

Abstract We investigate the statistical, dual‐spacecraft correlations of field‐aligned current (FAC) signatures between two Swarm spacecraft. For the first time, we infer the orientations of the current sheets of FACs by directly using the maximum correlations obtained from sliding data segments. The current sheet orientations are shown to broadly follow the mean shape of the auroral boundary for the lower latitudes and that these are most well ordered on the dusk side. Orientations at higher latitudes are less well ordered. In addition, the maximum correlation coefficients are explored as a function of magnetic local time and in terms of either the time shift ( δt ) or the shift in longitude ( δlon ) between Swarms A and C for various filtering levels and choice of auroral region. We find that the low‐latitude FACs show the strongest correlations for a broad range of magnetic local time centered on dawn and dusk, with a higher correlation coefficient on the dusk side and lower correlations near noon and midnight. The positions of maximum correlation are sensitive to the level of low‐pass filter applied to the data, implying temporal influence in the data. This study clearly reflects the two different domains of FACs: small‐scale (some tens of kilometers), which are time variable, and large‐scale (>50 km), which are rather stationary. The methodology is deliberately chosen to highlight the locations of small‐scale influences that are generally variable in both time and space. We may fortuitously find a potential new way to recognize bursts of irregular pulsations (Pi1B) using low‐Earth orbit satellites.

Noon

Dusk

Local time

Longitude

Current sheet

10.1029/2018ja025205

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Citations (7)

How to find magnetic nulls and reconstruct field topology with MMS data?

Journal of Geophysical Research Space Physics (2015)

H. S. Fu A. Vaivads Y. V. Khotyaintsev Vyacheslav Olshevsky M. André

Abstract In this study, we apply a new method—the first‐order Taylor expansion (FOTE)—to find magnetic nulls and reconstruct magnetic field topology, in order to use it with the data from the forthcoming MMS mission. We compare this method with the previously used Poincare index (PI), and find that they are generally consistent, except that the PI method can only find a null inside the spacecraft (SC) tetrahedron, while the FOTE method can find a null both inside and outside the tetrahedron and also deduce its drift velocity. In addition, the FOTE method can (1) avoid limitations of the PI method such as data resolution, instrument uncertainty ( Bz offset), and SC separation; (2) identify 3‐D null types ( A , B , As , and Bs ) and determine whether these types can degenerate into 2‐D ( X and O ); (3) reconstruct the magnetic field topology. We quantitatively test the accuracy of FOTE in positioning magnetic nulls and reconstructing field topology by using the data from 3‐D kinetic simulations. The influences of SC separation (0.05~1 d i ) and null‐SC distance (0~1 d i ) on the accuracy are both considered. We find that (1) for an isolated null, the method is accurate when the SC separation is smaller than 1 d i , and the null‐SC distance is smaller than 0.25~0.5 d i ; (2) for a null pair, the accuracy is same as in the isolated‐null situation, except at the separator line, where the field is nonlinear. We define a parameter ξ ≡ |( λ 1 + λ 2 + λ 3 )|/|λ| max in terms of the eigenvalues ( λ i ) of the null to quantify the quality of our method—the smaller this parameter the better the results. Comparing to the previously used parameter ( η ≡|∇ ⋅ B |/|∇ × B |), ξ is more relevant for null identification. Using the new method, we reconstruct the magnetic field topology around a radial‐type null and a spiral‐type null, and find that the topologies are well consistent with those predicted in theory. We therefore suggest using this method to find magnetic nulls and reconstruct field topology with four‐point measurements, particularly from Cluster and the forthcoming MMS mission. For the MMS mission, this null‐finding algorithm can be used to trigger its burst‐mode measurements.

Null (SQL)

10.1002/2015ja021082

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Citations (133)

First results of low frequency electromagnetic wave detector of TC-2/Double Star program

Annales Geophysicae (2005)

Jinbin Cao Z. X. Liu Junying Yang C. X. Yian Zixuan Wang

Abstract. LFEW is a low frequency electromagnetic wave detector mounted on TC-2, which can measure the magnetic fluctuation of low frequency electromagnetic waves. The frequency range is 8 Hz to 10 kHz. LFEW comprises a boom-mounted, three-axis search coil magnetometer, a preamplifier and an electronics box that houses a Digital Spectrum Analyzer. LFEW was calibrated at Chambon-la-Forêt in France. The ground calibration results show that the performance of LFEW is similar to that of STAFF on TC-1. The first results of LFEW show that it works normally on board, and that the AC magnetic interference of the satellite platform is very small. In the plasmasphere, LFEW observed the ion cyclotron waves. During the geomagnetic storm on 8 November 2004, LFEW observed a wave burst associated with the oxygen ion cyclotron waves. This observation shows that during geomagnetic storms, the oxygen ions are very active in the inner magnetosphere. Outside the plasmasphere, LFEW observed the chorus on 3 November 2004. LFEW also observed the plasmaspheric hiss and mid-latitude hiss both in the Southern Hemisphere and Northern Hemisphere on 8 November 2004. The hiss in the Southern Hemisphere may be the reflected waves of the hiss in the Northern Hemisphere.

Hiss

Plasmasphere

Geomagnetic latitude

10.5194/angeo-23-2803-2005

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Citations (54)

Simulating the Ring Current Proton Dynamics in Response to Radial Diffusion by Ultra‐Low‐Frequency (ULF) Waves

Geophysical Research Letters (2024)

Longxing Ma Yiqun Yu Wenlong Liu Jinbin Cao Yoshizumi Miyoshi

Abstract Radial diffusion (RD) induced by ULF waves can contribute to particle acceleration and scattering. Past global simulations that incorporate RD often use dipole magnetic fields, which could not realistically reveal the role of RD. To better understand the effects of RD and identify whether a background magnetic field model matters in understanding the ring current dynamics in response to RD, we simulate a storm event with different magnetic configurations using a global kinetic ring current model. Results indicate that RD can effectively diffuse protons of hundreds of keV to inner regions ( L ∼ 3.5), especially in recovery phase. Comparisons with in‐situ observations demonstrate that simulations with TS05 overall capture both the intensity and variations of proton fluxes with the aid of RD, whereas that with a dipole field significantly overestimates low‐L region fluxes. This study implies adopting realistic magnetic fields is important for correctly interpreting the role of RD.

Ring current

Intensity

10.1029/2023gl107326

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Citations (2)

Key Questions of Solar Wind–Moon Interaction

Space Science & Technology (2023)

Hui Zhang Jinbin Cao Yangting Lin Yong Wei P. R. Li

Key questions on solar wind–Moon interaction are reviewed. As the nearest celestial body to Earth, Moon’s space environment is distinctive to Earth’s mainly because of lack of a significant atmosphere/ionosphere and a global magnetic field. From a global respective, solar wind can bombard its surface, and the solar wind materials cumulated in the soil record the evolution of the Solar System. Many small-scale remanent magnetic fields are scattered over the lunar surface and, just as planetary magnetic fields protect planets, they are believed to divert the incident solar wind and shield the local lunar surface beneath, thus producing unique local surface environment that is critical to activities of human beings/facilities, thus providing unique landing sites to explore the origins of lunar swirls and remanent magnetic fields. Evidences have hinted that this local interaction, however, may be also distinct with the interacting scenario on planets, and the specific process has not been revealed because of lack of in situ observations in the near-Moon space or on the ground. The global and local solar wind interactions of the Moon represent 2 types of characteristic interaction of celestial bodies with stellar wind in deep space, i.e., the interactions of nonmagnetized bodies and of small-scale magnetized bodies, both of which may occur on asteroids and Mars. The deep-space celestial bodies, either difficult or impossible to reach for human beings or artificial satellites, are hard to measure, and the exploration of the Moon can reveal the mystery of stellar wind interaction on these bodies.

Mercury's magnetic field

10.34133/space.0060

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Citations (4)

Magnetospheric Physics in China

Chinese Journal of Space Science (2020)

Jinbin Cao Junying Yang

In the past two years, many progresses were made in Magnetospheric Physics by using the data of SuperMAG, Double Star Program, Cluster, THEMIS, RBSP, DMSP, DEMETER, NOAA, Van Allen probe, Swarm, MMS, ARTEMIS, MESSENGER, Fengyun, BeiDa etc., or by computer simulations. This paper briefly reviews these works based on papers selected from the 248 publications from January 2018 to December 2019. The subjects covered various sub-branches of Magnetospheric Physics, including geomagnetic storm, magnetospheric substorm, magnetic reconnection, solar wind-magnetosphere-ionosphere interaction, radiation belt, ring current, whistler waves, plasmasphere, outer magnetosphere, magnetotail, planetary magnetosphere, and technique.

Plasmasphere

Substorm

Ring current

Whistler

Van Allen Probes

10.11728/cjss2020.05.778

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Statistical analysis of earthward flow bursts in the inner plasma sheet during substorms

Journal of Geophysical Research Atmospheres (2009)

Yaroshevskaya A.D.Jinbin Cao R. Nakamura T. L. Zhang H. Rème

In this article, we study the velocity distribution, density, duration, and energy transport of earthward flow bursts in the inner plasma sheet (IPS) during three substorm phases using the data of Cluster in 2001 and 2002. The mean peak velocity of earthward flow bursts in recovery phases (390 km/s) is smaller than those in growth and expansion phases (490 and 520 km/s). The super earthward flow bursts (V > 1000 km/s) appear more frequently in the expansion phase. The average ion density of earthward flow bursts in the recovery phase is 0.14 cm −3 , much smaller than those in growth and expansion phases (0.28 and 0.21 cm −3 ), indicating that lobe reconnections most likely occur in the recovery phase. The average durations of earthward flow bursts in recovery phase are 48 s, smaller than those in growth and expansion phases (99 and 103 s), suggesting that the reconnections occurring in recovery phase are rather short‐lived. The earthward flow bursts in the expansion phase have largest capability of the transport of energy, about 7 times that in the recovery phase. Thus the earthward flow bursts in the expansion phase can produce largest impact effects to the inner magnetosphere.

Substorm

Plasma sheet

10.1029/2009ja014275

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Citations (41)