Binzheng Zhang

University of Hong Kong

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W. Lotko

High Altitude Observatory

J. G. Lyon

Dartmouth College

O. J. Brambles

Dartmouth College

M. Wiltberger

High Altitude Observatory

Jiuhou Lei

University of Science and Technology of China

Zhonghua Yao

University of Hong Kong

Wenbin Wang

High Altitude Observatory

Tong Dang

University of Science and Technology of China

Kareem Sorathia

Johns Hopkins University Applied Physics Laboratory

Yong Wei

Institute of Geology and Geophysics

Cooperative Institutions

Chinese Academy of Sciences

University of Science and Technology of China

Johns Hopkins University Applied Physics Laboratory

University of Colorado Boulder

NSF National Center for Atmospheric Research

Dartmouth College

High Altitude Observatory

University of Chinese Academy of Sciences

Shandong University

Peking University

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Transition from global to local control of dayside reconnection from ionospheric‐sourced mass loading

Journal of Geophysical Research Space Physics (2017)

Binzheng Zhang O. J. Brambles P. A. Cassak J. Ouellette M. Wiltberger

Abstract We have conducted a series of controlled numerical simulations to investigate the response of dayside reconnection to idealized, ionosphere‐sourced mass loading processes to determine whether they affect the integrated dayside reconnection rate. Our simulation results show that the coupled solar wind‐magnetosphere system may exhibit both local and global control behaviors depending on the amount of mass loading. With a small amount of mass loading, the changes in local reconnection rate affects magnetosheath properties only weakly and the geoeffective length in the upstream solar wind is essentially unchanged, resulting in the same integrated dayside reconnection rate. With a large amount of mass loading, however, the magnetosheath properties and the geoeffective length are significantly affected by slowing down the local reconnection rate, resulting in an increase of the magnetic pressure in the magnetosheath, with a significant reduction in the geoeffective length in the upstream solar wind and in the integrated dayside reconnection rate. In this controlled simulation setup, the behavior of dayside reconnection potential is determined by the role of the enhanced magnetic pressure in the magnetospheath due to magnetospheric mass loading. The reconnection potential starts to decrease significantly when the enhanced magnetic pressure alters the thickness of the magnetosheath.

Magnetosheath

10.1002/2016ja023646

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Citations (23)

Suppression of the Polar Tongue of Ionization During the 21 August 2017 Solar Eclipse

Geophysical Research Letters (2018)

Tong Dang Jiuhou Lei Wenbin Wang A. G. Burns Binzheng Zhang

Abstract It has long been recognized that during solar eclipses, the ionosphere‐thermosphere system changes greatly within the eclipse shadow, due to the rapid reduction of solar irradiation. However, the concept that a solar eclipse impacts polar ionosphere behavior and dynamics as well as magnetosphere‐ionosphere coupling has not been appreciated. In this study, we investigate the potential impact of the 21 August 2017 solar eclipse on the polar tongue of ionization (TOI) using a high‐resolution, coupled ionosphere‐thermosphere‐electrodynamics model. The reduction of electron densities by the eclipse in the middle latitude TOI source region leads to a suppressed TOI in the polar region. The TOI suppression occurred when the solar eclipse moved into the afternoon sector. The Global Positioning System total electron content observations show similar tendency of polar region total electron content suppression. This study reveals that a solar eclipse occurring at middle latitudes may have significant influences on the polar ionosphere and magnetosphere‐ionosphere coupling.

Solar eclipse

Eclipse

10.1002/2018gl077328

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Citations (28)

On the Relation Between Jupiter's Aurora and the Dawnside Current Sheet

Geophysical Research Letters (2023)

Y. B. Xu Zhonghua Yao Binzheng Zhang P. A. Delamere L. C. Ray

Abstract Jupiter's auroral emission is a spectacular phenomenon that provides insight into energy release processes related to the coupling of its magnetosphere and ionosphere. This energy release is influenced by solar wind conditions. Using joint observations from Juno and the Hubble Space Telescope (HST), we statistically investigate the relationship between auroral power and current sheet variations under different solar wind conditions. In this study, we reveal that during global main auroral brightening events that are closely connected to solar wind compressions, the dawn side current sheet is substantially thinner than during times when a quiet auroral morphology is present. Furthermore, the total current intensity in the current sheet is found to increase under solar wind compression conditions compared to the quiet period. These findings provide important observational evidence for how magnetospheric dynamics driven by solar wind behavior affect auroral activity, deepening our understanding of the coupling between Jupiter's magnetosphere and ionosphere.

Current sheet

Jupiter (rocket family)

Plasma sheet

Magnetosphere of Jupiter

10.1029/2023gl104123

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Citations (7)

Novel approaches to geospace particle transfer in the digital age: Progress through data science

Ryan McGranaghan Enrico Camporeale K. A. Lynch J. W. Gjerloev Téo Bloch

Earth and Space Science Open Archive posterOpen AccessYou are viewing the latest version by default [v1]Novel approaches to geospace particle transfer in the digital age: Progress through data scienceAuthors Ryan McGranaghan iD Enrico Camporeale Kristina Lynch Jesper Gjerloev iD Téo Bloch iD Spencer Hatch iD Binzheng Zhang Pete Riley iD Mathew Owens iD Yuri Shprits Irina Zhelavskaya iD Susan Skone See all authors Ryan McGranaghaniDCorresponding AuthorASTRA LLCiDhttps://orcid.org/0000-0002-9605-0007view email addressThe email was not providedcopy email addressEnrico CamporealeNOAAview email addressThe email was not providedcopy email addressKristina LynchDartmouth Collegeview email addressThe email was not providedcopy email addressJesper GjerloeviDJHU APLiDhttps://orcid.org/0000-0002-7277-9004view email addressThe email was not providedcopy email addressTéo BlochiDUniversity of ReadingiDhttps://orcid.org/0000-0001-6017-1619view email addressThe email was not providedcopy email addressSpencer HatchiDUniversity of BergeniDhttps://orcid.org/0000-0001-7412-4936view email addressThe email was not providedcopy email addressBinzheng ZhangHong Kong Universityview email addressThe email was not providedcopy email addressPete RileyiDPredictive Science Inc.iDhttps://orcid.org/0000-0002-1859-456Xview email addressThe email was not providedcopy email addressMathew OwensiDUniversity of ReadingiDhttps://orcid.org/0000-0003-2061-2453view email addressThe email was not providedcopy email addressYuri ShpritsUniversity of California Los Angelesview email addressThe email was not providedcopy email addressIrina ZhelavskayaiDGFZ PotsdamiDhttps://orcid.org/0000-0002-7029-5372view email addressThe email was not providedcopy email addressSusan SkoneUniversity of Calgaryview email addressThe email was not providedcopy email address

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10.1002/essoar.10501929.1

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Thank You to Our 2022 Peer Reviewers

AGU Advances (2023)

Susan Trumbore Ana P. Barros T. W. Becker M. Bayani Cardenas Eric A. Davidson

Abstract The editorial board of AGU Advances thanks the individuals who reviewed for the journal in 2022.

10.1029/2023av000974

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Simulating the Solar Wind‐Magnetosphere Interaction During the Matuyama‐Brunhes Paleomagnetic Reversal

Geophysical Research Letters (2022)

Fan Gong Yiqun Yu Jinbin Cao Yong Wei Jiawei Gao

Abstract During a paleomagnetic reversal, Earth's geomagnetic field is about 10% of today's magnitude and its topology is far more complex than dipolar. Revealing the solar wind energy transmission during the reversal is of importance for understanding the historic space environment. Using a global magnetohydrodynamic model implemented with a data‐reconstructed time‐dependent paleomagnetic field, this study simulates the solar wind‐magnetosphere interactions during the last Matuyama‐Brunhes reversal that occurred about 780,000 years ago. As the magnetosphere shrinks in the midst of the reversal, the stand‐off distance of the subsolar magnetopause approaches as close as 3 Re. Moreover, multiple magnetic reconnection sites emerge due to the irregular geomagnetic configuration, opening up many channels on the magnetopause surface for the solar wind to directly access. The power transmission efficiency through the magnetopause increases to 18%.

Space Weather

Geomagnetic reversal

10.1029/2021gl097340

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Citations (5)

Temporary consolidation and packaging of fragile cultural relics at underwater archaeological sites to maintain their original state during extraction

Archaeometry (2020)

Xueqiang Chen Lan Xie Fangwei Wang Yiping Wu Binzheng Zhang

The flexible sponge/epoxy composite can wrap underwater artefacts in any shape and forms a protective shell after curing, thus effectively wrapping and reinforcing the artefacts. However, the hydroscopicity of the sponge itself limits the underwater application of the sponge/epoxy composite. In this study, a novel polyurethane sponge was prepared by modified with super‐hydrophobic multi‐wall carbon nanotubes (SH‐MWCNTs@PU sponge). Compared with the pristine PU sponge, the water‐contact angle on the surface of SH‐MWCNTs@PU sponges increased from 103.3 ± 1.82 to 152.6 ± 1.54 o , and oily epoxy resin was able to cover the surface completely. The study shows that when SH‐MWCNTs@PU sponges/epoxy resin composite material is used underwater, it prevents both water from entering the sponge and also the inside epoxy resin from overflowing into the water. Moreover, the composite materials have excellent toughness after reinforcement under water (flexural strength = 3.56 MPa) and the soft sponges can be moulded to wrap any type of underwater artefacts. In the laboratory, when taking a broken, three‐dimensional blue‐and‐white porcelain pot as a research subject, the entire retrieval process—temporary stabilization, packaging, extraction and reinforcement material removal—was simulated to evaluate systematically all the technological aspects of safely excavating fragile underwater relics.

Sponge

Consolidation

10.1111/arcm.12571

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Citations (11)

Magnetosphere Sawtooth Oscillations Induced by Ionospheric Outflow

Science (2011)

O. J. Brambles W. Lotko Binzheng Zhang M. Wiltberger J. G. Lyon

The sawtooth mode of convection of Earth's magnetosphere is a 2- to 4-hour planetary-scale oscillation powered by the solar wind-magnetosphere-ionosphere (SW-M-I) interaction. Using global simulations of geospace, we have shown that ionospheric O(+) outflows can generate sawtooth oscillations. As the outflowing ions fill the inner magnetosphere, their pressure distends the nightside magnetic field. When the outflow fluence exceeds a threshold, magnetic field tension cannot confine the accumulating fluid; an O(+)-rich plasmoid is ejected, and the field dipolarizes. Below the threshold, the magnetosphere undergoes quasi-steady convection. Repetition and the sawtooth period are controlled by the strength of the SW-M-I interaction, which regulates the outflow fluence.

Sawtooth wave

Outflow

Plasmoid

Oscillation (cell signaling)

Substorm

Field line

10.1126/science.1202869

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Citations (118)

Periodicities and Plasma Density Structure of Jupiter's Dawnside Magnetosphere

Journal of Geophysical Research Planets (2023)

A. A. Schok P. A. Delamere B. Mino P. A. Damiano Binzheng Zhang

Abstract Ability to quantify variations in magnetic field topology and density within Jupiter's magnetosphere is an important step in understanding the overall structure and dynamics. The Juno spacecraft has provided a rich data set in the dawnside magnetosphere. The recent Grid Agnostic MHD for Extended Research Applications (GAMERA) global simulation study by Zhang et al. (2021, https://doi.org/10.1126/sciadv.abd1204 ) showed a highly structured plasmadisc with closed magnetic field lines mapped between the outer dawn‐tail flank and the high‐latitude polar region. To test these model predictions, we examined Juno's magnetic field data and electron/energetic particle data to categorize portions of orbits 1–15 into one of three regions based on plasma confinement: the flux pileup region, the intermediate region, and the plasmadisc region. For each region we examined periodicities from magnetic field fluctuations and particle density fluctuations on the 1–10 hr time scale. Periodicities on this time scale could relate to internal (e.g., plasmadisc structure) or external processes (e.g., Kelvin‐Helmholtz vortices). Similar analysis was performed on the GAMERA simulation with the data split into two regions, an outer (150 > R > 60) region and an inner ( R < 60) region. Finally, using published density moments from Huscher et al. (2021, https://doi.org/10.1029/2021JA029446 ), we compared the relative density variations of the Juno moments and the GAMERA simulation to further understand the overall structure and dynamics of the plasmadisc. The agreement between data and simulation supports the existence of such a highly structured plasmadisc.

10.1029/2022je007637

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Citations (11)

The role of ionospheric O⁺ outflow in the generation of earthward propagating plasmoids

Journal of Geophysical Research Space Physics (2015)

Binzheng Zhang O. J. Brambles W. Lotko J. Ouellette J. G. Lyon

Abstract Earthward propagating plasmoids in the Earth's magnetotail have been observed by satellites. Using a multifluid global magnetosphere simulation, earthward propagating plasmoids are reproduced when ionospheric O + outflow is included in the global simulation. Controlled simulations show that without ionospheric outflow, the plasmoids generated in the magnetotail during a substorm‐steady magnetospheric convection cycle only propagate tailward. With ionospheric outflow, earthward plasmoids can be induced through the modification of magnetotail reconnection at multiple X lines. When multiple X lines form in the magnetotail, plasmoids may be trapped between multiple reconnection sites. When magnetic reconnection rate is reduced at the near‐Earth X line by the presence of ionospheric O + , the earthward exhaust flow of reconnection occurring at the midtail X line forces the plasmoid to propagate earthward. The propagation speed and spatial size of the simulated earthward plasmoid are consistent with observations from the Cluster satellites.

Plasmoid

Substorm

Outflow

10.1002/2015ja021667

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Citations (11)