His research is focused on the interpretation and modeling of MHD wave activity in the solar atmosphere, the design of inversion and model comparison tools for remote sensing of the physical conditions and the dynamics of solar atmospheric plasmas, and the study of wave based plasma heating mechanisms. He aims at further developing the fields of seismology and wave heating of the solar atmosphere in combination with observations from space solar missions.
My research about the Sun lies in studying the variations in the structure and dynamics of the Sun over time-scales. I study other stars since I am interested in the properties of stellar materials. The study of stars other than the Sun also allows me to study the structure and evolution of the Galaxy; it also informs my study of the Sun. I specialize in studying solar and stellar properties using data on stellar oscillations.
Lockheed Martin Solar & Astrophysics Laboratory, 3251 Hanover St, Palo Alto, CA 94304, USA
I study the physical processes occurring on the Sun with large scale numerical simulations and observations from telescopes like those onboard NASA's Solar Dynamics Observatory, Interface Region Imaging Spectrograph and the Japanese Hinode mission.
Solar and stellar astrophysics; acceleration of stellar winds; heating of stellar coronae and chromospheres; plasma physics and kinetic theory of waves and turbulence; rotating hot (O, B, Wolf-Rayet) stars; circumstellar fluid dynamics; radiative transfer and spectroscopy.
Solar and astrophysical magnetohydrodynamics; dynamics of rising magnetic flux tubes in the solar interior; physics of solar active region formation; interaction of solar p-modes with active region magnetic flux tubes; helioseismology.
My scientific interests lie in understanding the large scale structure and dynamics of the heliospheric magnetic field, the solar wind in which it is embedded, and their relationship and response to the structures present in the Sun’s atmosphere, the corona.
Core research interests include understanding the origin, acceleration, and propagation of cosmic rays, and other charged-particle species in the magnetic fields of space, and general topics in space plasma physics, and astrophysics.
He develops physics-based theoretical and computational models which are used to interpret in situ spacecraft observations. He is interested in the general properties of solar, interplanetary, and galactic magnetic fields.
Star formation, accretion, circumstellar disks, outflows; The "Young Sun" and its environment; Magnetic activity in young stars and stellar environments, coronal heating; Plasma astrophysics and magnetohydrodynamics in stellar plasmas; Radio interferometry, infrared-/mm-/sub-mm astronomy, X-ray spectroscopy
Atmospheric radiative transfer; Climate modelling; Radiation codes for numerical models; Interaction of radiation, dynamics and photochemistry in the middle atmosphere; Satellite remote sensing of cloud, aerosol and ocean colour; Radiative forcing of climate change; Solar irradiance variability and its influence on the structure of the lower and middle atmosphere; 3D radiative transfer in inhomogeneous cloud.
My research field is helio- and asteroseismology, which is the study of oscillations (vibrations) in the Sun and in distant stars. Other topics of my research include stellar convection modelling and the determination of stellar chemical abundances and ages.
Solar wind-magnetosphere coupling, transient magnetic reconnection, the circulation of plasma populations of solar and ionospheric origins in the magnetosphere, cosmic rays, evolution of solar magnetic fields, space weather and space climate change
Dr. Longcope conducts theoretical research into the basic physics of
magnetic fields in ionized plasmas and the application of these concepts to magnetic fields on the Sun. He has studied the storage
and release of magnetic energy in the Sun's corona through a process known as reconnection. He has also
studied the rise of slender strands of magnetic field from deep within the Sun up to the solar surface.
Computational MHD and code development, Solar Prominences, Coronal Heating, Magnetic Flux Transport and Magnetofrictional Relaxation Simulations, Stellar Magnetic Fields, Sun's Open Magnetic Flux and Solar Terrestrial
I combine theoretical modeling based on numerical simulations and observational data analysis to study physical processes operating in the Sun such as: Emergence of magnetic fields into the solar atmosphere (flux emergence); Formation of magnetic structures in the solar atmosphere (prominences/filaments, sigmoids); Dissipation of magnetic fields in the solar atmosphere (flares, jets, coronal heating); Ejection of magnetic fields toward the interplanetary space (solar winds, coronal mass ejections)
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany; now at Institute for Experimental and Applied Physics, Christian Albrechts University Kiel, Germany
His research covers the physics of the solar corona and solar wind, and generally of space plasmas. He has been active in data analysis as well as theory and modelling. He has been co investigator of many experiments, among them the EUV spectrometer SUMER on SOHO and the SECCHI instrument on STEREO. He proposed the Solar Orbiter mission, which was selected by ESA to fly around 2014.
I'm interested in astrophysical fluid dynamics and magnetohydrodymanics, particularly as it applies to the interior of the sun and other stars. Most of my recent work focuses on high-resolution numerical simulations of convection, turbulence, and shear in the solar interior and the implications all this has for solar dynamo theory and for detectable surface flows such as differential rotation and solar sub-surface weather. I've also done some work on turbulence and waves in interstellar molecular clouds.
My research interests are in the solar physics, astrophysics and nonlinear wave theory. The key word in all my work is a wave (for me, it is something which can propagate somewhere). Particularly, I deal with magnetohydrodynamic (MHD) waves, which are believed to be responsible for a number of astrophysical phenomena and are observed in the atmosphere of the Sun, solar wind and magnetosphere of the Earth (However, it seems that they can be found everywhere in the Universe, where there is a plasma penetrated by the magnetic field). Propagating through an inhomogeneous, non-stationary, nonlinear and sometimes active medium, such as the space plasma, MHD waves gain extremally interesting new properties leading to a number of amazing physical phenomena, like the existence of solitons, negative energy effects, self-organisation and many others.
Solar plasma physics; Magnetohydrodynamics; Fluid waves and instabilities; Kinetic waves and instabilities; Numerical MHD; Numerical hybrid kinetic models; Solar active regions; Coronal Mass Ejections; Coronal heating; Solar wind; Analysis of satellite EUV observations
X-ray and UV astronomy. Solar and stellar coronal physics: dynamic phenomena in confined structures; data analysis and modeling of structuring and dynamics of the solar corona; modeling and diagnostics of stellar flares and coronae; study of the Sun as an X-ray star. Astrophysics of binary systems and interstellar medium: variability of extragalactic X-ray binary systems; thermal stability of stratified atmospheres; interaction of supernova remnants with interstellar clouds; circumstellar matter in star forming regions. Numerical astrophysics: hydrodynamic and MHD codes; parallel high performance computing.
He focuses his research on modeling of MHD processes in the solar interior, coupled models of the differential rotation, meridional flow, and large-scale dynamo, addressing non-kinematic effects and cycle variations of the solar differential rotation (torsional oscillations).
My research focuses on astrophysical fluid and plasma dynamics, notably solar physics, turbulent convection, MHD and dynamo theory, accretion disk turbulence, microinstabilities in magnetized plasmas, and pulsations of magnetized stars.
My main research interests are three-dimensional simulations of convection and magneto-convection in the Sun, and one-dimensional radiation-hydrodynamics of waves and non-equilibrium radiation in the solar atmosphere.
University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, U.K. and Konkoly Observatory of Hungarian Academy of Sciences, Budapest, Hungary and Observatoire de Paris, LESIA, FRE 2461(CNRS), F-92195 Meudon Principal Cedex, France
Theory and observations of magnetohydrodynamic wave phenomena in the solar corona and the determination of physical coronal plasma parameters from observations of MHD wave characteristics. Application of image-analysis techniques to solar image data.
particle acceleration in solar flares (mainly using RHESSI and radio data), large-scale coronal waves and shocks, conditions in the quiet and active region corona, multiwavelength observations (from radio to hard X-rays…), space weather
My professional interests include solar coronal physics, coronal mass ejections (CMEs) and space weather, which includes a heavy dose of halo CMEs and their heliospheric characteristics and geoeffectiveness.
Active regions, Coronal holes, Magnetic fields, Coronal heating, Solar image processing, Tomography, Stereoscopy, Magnetic Reconnection, Helmet streamer, Solar Wind, Coronal Mass Ejections (CMEs), Basic Plasmaphysics (MHD, Kinetics), Optimization methods
Naval Research Laboratory, Space Science Division, Washington, DC 20375, U.S.A.
My primary research interests involve observational studies of the outer atmosphere of cool stars using UV, EUV, X-ray, and radio emissions from these stars. I am also interested in the local interstellar medium and its interactions with the winds of late-type stars. The Sun certainly falls within my purview, as I have analyzed observations of the Sun and heliosphere, in addition to my work on cool stars in general.
Department of Mathematical Sciences, Durham University, Science Laboratories, South Road, Durham DH1 3LE, UK
My main interest is magnetohydrodynamics (MHD), particularly the structure and evolution of the Sun's magnetic field. I focus on problems which are nonlinear, three-dimensional, time-dependent, or all three. I apply a mixture of numerical and analytical modelling.