A5001420388- Solar and Space Plasma Dynamics
- Ionosphere and magnetosphere dynamics
- Geomagnetism and Paleomagnetism Studies
- Astro and Planetary Science
- Stellar, planetary, and galactic studies
- Geophysics and Gravity Measurements
- MicroRNA in disease regulation
- Solar Radiation and Photovoltaics
- Magnetic confinement fusion research
- Gamma-ray bursts and supernovae
- BRCA gene mutations in cancer
- Nutrition, Genetics, and Disease
- Astrophysics and Cosmic Phenomena
- Cancer Genomics and Diagnostics
- Mobile Ad Hoc Networks
- Atmospheric Ozone and Climate
- Cancer-related molecular mechanisms research
- High-Energy Particle Collisions Research
- Genetic Associations and Epidemiology
- Earthquake Detection and Analysis
- Cosmology and Gravitation Theories
- Fluid Dynamics and Turbulent Flows
- Cooperative Communication and Network Coding
- Cancer Risks and Factors
- Extracellular vesicles in disease
University of Alabama in Huntsville
2016-2025
Tongde Hospital of Zhejiang Province
2022-2024
Shanghai Jiao Tong University
1995-2024
Shenzhen Center for Disease Control and Prevention
2024
Hainan University
2024
Jiangxi Academy of Sciences
2023-2024
General Hospital of Shenyang Military Region
2022-2023
University of Calgary
2023
Hebei University
2023
ShanghaiTech University
2020-2023
The Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Probe Plus is a four sensor instrument suite that provides complete measurements of the electrons ionized helium hydrogen constitute bulk solar wind coronal plasma. SWEAP consists Cup (SPC) Analyzers (SPAN). SPC Faraday looks directly at Sun measures ion electron fluxes flow angles as function energy. SPAN an electrostatic analyzer (ESA) ram side SPP (SPAN-A) ESA anti-ram (SPAN-B). SPAN-A has time flight section enables it...
Abstract Full-disk measurements of the solar magnetic field by Helioseismic and Magnetic Imager (HMI) are often used for extrapolations, but its limited spatial spectral resolution can lead to significant errors. We compare HMI data with observations NOAA 12104 Hinode Spectropolarimeter (SP) derive a scaling curve strength, B . The SP in Fe i lines at 630 nm were inverted SIR code. find that Milne–Eddington inversion underestimates line-of-sight flux, Φ, all granulation surroundings an...
We develop a new approach for determining the orientation of axis ( z ) finite‐β magnetic flux ropes from single‐spacecraft data. It consists an optimization procedure based on two‐dimensional magnetohydrostatic theory. From requirement that transverse pressure, P t = p + B 2 /2μ 0 , be function calculated potential, A alone, optimal is found. Benchmark studies using analytical rope solutions show feasibility this axis‐determination approach. Two cloud events, 18 October 1995 and 9 January...
We present the first quantitative comparison between total magnetic reconnection flux in low corona wake of coronal mass ejections (CMEs) and clouds (MCs) that reach 1 AU 2-3 days after CME onset. The is measured from flare ribbons, MC computed using situ observations at AU, all ranging 1020 to 1022 Mx. It found for nine studied events which association flares, CMEs, MCs identified, correlated with Φr. Further, poloidal (azimuthal) Φp comparable Φr, toroidal (axial) Φt a fraction Events...
On 29–30 October 2003 the Solar Wind Electron Proton Alpha Monitor (SWEPAM) instrument on Advanced Composition Explorer (ACE) spacecraft measured solar wind speeds in excess of 1850 km/s, some highest ever directly wind. These were observed following two large coronal mass ejection (CME) driven shocks. Surprisingly, despite unusually high speeds, many other parameters not particularly unusual comparison with transient events. The magnetic field reached −68 nT, a but unprecedented value....
On the basis of a recently developed nonlinear guiding center theory for perpendicular spatial diffusion coefficient κ ⊥ used to describe transport energetic particles, we construct model diffusive particle acceleration at highly shocks, i.e., shocks whose upstream magnetic field is almost orthogonal shock normal. We use investigate anisotropy and injection energy all obliquities, finding that 1 AU, example, parallel can inject protons with equal facility. It only very high energies are...
Abstract Solar eruptions are well-recognized as major drivers of space weather but what causes them remains an open question. Here we show how eruption is initiated in a non-potential magnetic flux-emerging region using magnetohydrodynamic modelling driven directly by solar magnetograms. Our model simulates the coronal field following long-duration quasi-static evolution to its fast eruption. The morphology resembles set extreme ultraviolet images for whole process. Study suggests that this...
Current magnetohydrodynamic (MHD) simulations of the initiation solar eruptions are still commonly carried out with idealized magnetic field models, whereas realistic coronal prior to can possibly be reconstructed from observable photospheric field. Using a nonlinear force-free extrapolation sigmoid eruption in AR 11283 as initial condition MHD model, we successfully simulate process event, is confirmed by remarkable resemblance SDO/AIA observations. Analysis pre-eruption reveals that...
Abstract The thermal plasma beta in the solar wind and corona is of order <?CDATA $\beta \sim 1$?> \ll . Zank et al. developed 2D slab turbulence transport model equations using nearly incompressible (NI) theory. We solve NI MHD coupled for inhomogeneous from 1 to 75 au, compare numerical solutions Voyager 2 observations. find that (1) turbulent energies are larger than throughout heliosphere; (2) decrease more slowly within ∼4 while increase flatten outer (3) normalized cross-helicity...
Zank et al. developed a turbulence transport model for low-frequency incompressible magnetohydrodynamic (MHD) in inhomogeneous flows terms of the energy corresponding to forward and backward propagating modes, residual energy, correlation lengths length energy. We apply super-Alfvénic solar wind i.e., solve coupled equations two cases, first being heliosphere from 0.29 5 AU with without Alfvén velocity, second "entire" 100 absence velocity. The shows that (1) shear driving is responsible...
We present an end-to-end Neural Human Renderer (NHR) for dynamic human captures under the multi-view setting. NHR adopts PointNet++ feature extraction (FE) to enable robust 3D correspondence matching on low quality, reconstructions. To render new views, we map features onto target camera as a 2D and employ anti-aliased CNN handle holes noises. Newly synthesized views from can be further used construct visual hulls textureless and/or dark regions such black clothing. Comprehensive experiments...
Abstract The solar cycle dependence of various turbulence quantities and cosmic-ray (CR) diffusion coefficients is investigated by using OMNI 1 minute resolution data over 22 years. We employ Elsässer variables z ± to calculate the magnetic field energy correlation lengths for both inwardly outwardly directed interplanetary (IMF). present temporal evolution large-scale wind (SW) plasma small-scale fluctuations. Based on these observed quantities, we study influence activity CR parallel...
Abstract The possibility that charged particles are accelerated statistically in a “sea” of small-scale interacting magnetic flux ropes the supersonic solar wind is gaining credence. In this Letter, we extend Zank et al. statistical transport theory for nearly isotopic particle distribution by including an escape term corresponding to loss from finite acceleration region. Steady-state 1D solutions both velocity function and differential intensity derived. We show Ulysses observations...
We recover two‐dimensional magnetic structures of small‐scale flux ropes in the solar wind from WIND spacecraft data by solving plane Grad‐Shafranov equation as a spatial initial value problem. The cross‐sections two recovered show nested non‐circular loops transverse field lines rather than concentric circles. expected helical structure is recovered, albeit with significant distortions axial symmetry. rope are self‐consistent, non‐force free, magnetohydrostatic equilibria. Their...
We present direct evidence that magnetic clouds (MCs) have highly flattened and curved cross section resulting from their interaction with the ambient solar wind. Lower limits on transverse size are obtained for three MCs observed by ACE Ulysses latitudinal separation between two spacecraft, ranging 40° to 70°. The cross‐section aspect ratio of is estimated be no smaller than 6:1. offer a simple model extract radius curvature section, based elevation angle MC normal distributed over...
We develop a realistic and time-varying model that satisfies both the Voyager 1 (V1) 2 (V2) observed crossing times locations of termination shock (TS) simultaneously by performing three-dimensional (3D) magnetohydrodynamic (MHD) simulations using total variation diminishing (TVD) scheme includes effects neutral particles. Daily values solar-wind speed density V2 are used at every simulation step so short-term dynamical reproduced. Before dynamic simulation, we generate 3D stationary...
We present a comprehensive study of the formation and eruption an active region (AR) sigmoid in AR 11283. To follow quasi-static evolution coronal magnetic field, we reconstruct time sequence static fields using recently developed nonlinear force-free field model constrained by vector magnetograms. A detailed analysis compared with observations suggests following scenario for region. Initially, new bipole emerges into negative polarity preexisting bipolar AR, forming null-point topology...
We study the physical mechanism of a major X-class solar flare that occurred in super NOAA active region (AR) 12192 using data-driven numerical magnetohydrodynamic (MHD) modeling complemented with observations. With evolving magnetic fields observed at surface as bottom boundary input, we drive an MHD system to evolve self-consistently correspondence realistic coronal evolution. During two-day time interval, modeled field has been slowly stressed by photospheric evolution,which gradually...
Abstract We present unique and additional observational evidence for the self-generation of small-scale coherent magnetic flux rope structures in solar wind. Such with durations between 9 361 minutes are identified from Wind situ spacecraft measurements through Grad–Shafranov (GS) reconstruction approach. The event occurrence counts on order 3500 per year average have a clear solar-cycle dependence. build database ropes 20 yr worth data. show power-law distribution wall-to-wall time...
The magnetic flux rope is among the most fundamental configurations in plasma. Although its presence after solar eruptions has been verified by spacecraft measurements near Earth, formation on Sun remains elusive, yet critical to understanding a broad spectrum of phenomena. Here we study dynamic during classic two-ribbon flare. Its feet are identified unambiguously with conjugate coronal dimmings completely enclosed irregular bright rings, which originate and expand outward from far ends...