A5038923330- Computational Fluid Dynamics and Aerodynamics
- Fluid Dynamics and Turbulent Flows
- Solar and Space Plasma Dynamics
- Gas Dynamics and Kinetic Theory
- Ionosphere and magnetosphere dynamics
- Astro and Planetary Science
- Advanced Numerical Methods in Computational Mathematics
- Meteorological Phenomena and Simulations
- Architecture, Modernity, and Design
- Plasma and Flow Control in Aerodynamics
- Geomagnetism and Paleomagnetism Studies
- Planetary Science and Exploration
- Laser-Plasma Interactions and Diagnostics
- Rocket and propulsion systems research
- Aerodynamics and Acoustics in Jet Flows
- Lattice Boltzmann Simulation Studies
- Architecture and Cultural Influences
- Spacecraft and Cryogenic Technologies
- Organometallic Complex Synthesis and Catalysis
- Cyclopropane Reaction Mechanisms
- Fluid Dynamics and Vibration Analysis
- Geophysics and Gravity Measurements
- Gamma-ray bursts and supernovae
- Atmospheric Ozone and Climate
- Architecture and Computational Design
University of Michigan
2007-2021
University of Colorado Boulder
2021
BD Technologie (United States)
2013
Stanford University
2009
University of California, Santa Barbara
2009
University of California, Berkeley
2009
University of Illinois Urbana-Champaign
2009
American Institute of Aeronautics and Astronautics
2003
W. M. Keck Foundation
1997-2001
Glenn Research Center
1995
The Space Weather Modeling Framework (SWMF) provides a high‐performance flexible framework for physics‐based space weather simulations, as well various physics applications. SWMF integrates numerical models of the Solar Corona, Eruptive Event Generator, Inner Heliosphere, Energetic Particles, Global Magnetosphere, Radiation Belt, Ionosphere Electrodynamics, and Upper Atmosphere into coupled model. components can be represented with alternative models, any physically meaningful subset used....
A parallel adaptive mesh refinement (AMR) finite‐volume scheme for predicting ideal MHD flows is used to simulate the initiation, structure, and evolution of a coronal mass ejection (CME) its interaction with magnetosphere‐ionosphere system. The simulated CME driven by local plasma density enhancement on solar surface background initial state corona wind represented newly devised “steady state” solution. solution has been constructed provide reasonable description time‐averaged conditions...
We present a three‐dimensional (3‐D) numerical ideal magnetohydrodynamics (MHD) model describing the time‐dependent expulsion of coronal mass ejection (CME) from solar corona propagating to 1 astronomical unit (AU). The simulations are performed using Block Adaptive Tree Solar‐Wind Roe Upwind Scheme (BATS‐R‐US) code. begin by developing global steady‐state that possesses high‐latitude holes and helmet streamer structure with current sheet at equator. Archimedean spiral topology...
A spectral collocation and matrix eigenvalue method is used to study the linear stability of trailing line vortex model Batchelor. For both inviscid viscous problem, entire unstable region in swirl/axial wavenumber parameter space mapped out for various azimuthal wavenumbers m. In case, non-axisymmetric perturbation with m = 1 has an larger extent than any other, unusual two-lobed structure; also, location numerical value maximum disturbance growth rate previously reported this case are...
In this paper, a method is developed for designing multi-stage schemes that give optimal damping of highfrequencies given spatial-differencing operator. The objective the to design combine well with multi-grid acceleration. are tested on nonlinear scalar equation, and compared Runge-Kutta maximum stable time-step. optimally smoothing perform better than schemes, even single grid. analysis extended Euler equations in one space-dimension by use characteristic time-stepping, which preconditions...
The results of a three‐dimensional adaptive magnetohydrodynamic (MHD) model the interaction magnetized solar wind with very local interstellar medium in presence neutral hydrogen are presented. interplanetary magnetic field is approximated by Parker spiral, and direction taken to be arbitrary. It demonstrated that has pronounced effect on structure global heliosphere. In particular, it shown shocked significantly depends field. This mainly manifested distances heliospheric boundaries shape...
We present the results of model calculations using a multispecies MHD interaction solar wind with Mars. The three ions considered are H + , O 2 and representing two major ionospheric ion species, respectively. indicate that presence hot oxygen corona does not, within resolution accuracy model, lead to any significant effect on dayside bow shock ionopause positions. Next trans‐terminator fluxes escape down tail were calculated neglecting effects crustal magnetic field. flux values consistent...
We present a three‐dimensional (3‐D) numerical ideal magnetohydrodynamics (MHD) model, describing the time‐dependent expulsion of plasma and magnetic flux from solar corona that resembles coronal mass ejection (CME). begin by developing global steady‐state model wind gives reasonable description conditions near minimum. The field possesses high‐latitude holes closed lines at low latitudes in form helmet streamer belt with current sheet equator. further reproduce fast slow speed high...
A Cartesian cell-based approach for adaptively refined solutions of the Euler and Navier-Stokes equations in two dimensions is presented. Grids about geometrically complicated bodies are generated automatically, by recursive subdivision a single cell encompassing entire flow domain. Where resulting cells intersect bodies, polygonal cut created using modified polygon-clipping algorithms. The grid stored binary tree data structure that provides natural means obtaining cell-to-cell connectivity...
First results of a three‐dimensional multiscale MHD model the interaction an expanding cometary atmosphere with magnetized solar wind are presented. The starts supersonic and super‐Alfvènic far upstream comet (25 Gm nucleus) arbitrary interplanetary magnetic field orientation. is continuously mass loaded ions originating from 10‐km size nucleus. effects photoionization, electron impact ionization, recombination, ion‐neutral frictional drag taken into account in model. governing equations...
Most high-energy solar energetic particles are believed to be accelerated at shock waves driven by coronal mass ejections (CMEs). The acceleration process strongly depends on the geometry and structure of sheath that forms behind shock. In an effort understand time evolution such CME-driven shocks their relevance particle acceleration, we investigate interaction a fast CME with ambient wind means three-dimensional numerical ideal MHD model. Our global steady state model possesses...
X-ray emission was discovered in comet Hyakutake (C/1996 B2) by the Röntgen satellite 1996, and these emissions were attributed to excitation of high charge state solar wind ions due electron capture from cometary molecules or atoms. Using plasma flow coma calculated a three-dimensional adaptive magnetohydrodynamic model, density distribution resulting x-ray computed. The High Resolution Imager count rate 4.4 per second spatial agree with observations. A detailed energy spectrum x-rays is...
We describe the CRASH (Center for Radiative Shock Hydrodynamics) code, a block adaptive mesh code multi-material radiation hydrodynamics. The implementation solves diffusion model with gray or multigroup method and uses flux limited approximation to recover free-streaming limit. electrons ions are allowed have different temperatures we include electron heat conduction. hydrodynamic equations solved in Eulerian frame by means of conservative finite volume discretization either one, two,...
The testing of aeroelastically and aerothermoelastically scaled wind-tunnel models in hypersonic flow is not feasible; thus, computational aeroelasticity aerothermoelasticity are essential to the development vehicles.Several fundamental issues this area examined by performing a systematic study aeroelastic aerothermoelastic behavior three-dimensional configuration.Specifically, flutter boundary low-aspect-ratio wing, representative fin or control surface on vehicle, studied over range...
The solar wind‐magnetosphere interaction for northward interplanetary magnetic field (IMF) is studied using a newly developed three‐dimensional adaptive mesh refinement (AMR) global MHD simulation model. simulations show that north‐ward IMF the magnetosphere essentially closed. Reconnection between and magnetospheric limited to finite regions near cusps. When reconnection process forms closed lines on day side, wind plasma trapped these reconnected becomes part of low‐latitude boundary layer...