'Density profiles' presentation slideshows

Clusters and groups of galaxies

1.03k views • 80 slides

Lipid Bilayer Simulations: Force fields, Simulation and Analysis

Lipid Bilayer Simulations: Force fields, Simulation and Analysis. Jeffery B. Klauda. Model Yeast Membrane. Chemical Structure of Lipids. Lipids. Complex biomolecules. Contain a fatty acid chains and head group. Classified into 8 categories 1. Fatty acyls. Glycerolipids.

670 views • 39 slides

The EURIPOS Project: Eu ropean R esearch Network of I onospheric and P lasmaspheric O bservation S ystems

The EURIPOS Project: Eu ropean R esearch Network of I onospheric and P lasmaspheric O bservation S ystems. Anna Belehaki National Observatory of Athens, Greece. Fifth European Space Weather Week, Brussels, 17-21 November 2008. The idea.

375 views • 29 slides

337 views • 28 slides

Two problems with gas discharges

Two problems with gas discharges. Anomalous skin depth in ICPs Electron diffusion across magnetic fields. Problem 1: Density does not peak near the antenna (B = 0). Problem 2: Diffusion across B. Classical diffusion predicts slow electron diffusion across B.

420 views • 27 slides

Inflation + ?CDM Model = Cosmology Galaxies Formation

416 views • 26 slides

Swarming and Contagion

Swarming and Contagion. Andrea Bertozzi Department of Mathematics, UCLA. Thanks to support from ARO, NSF, and ONR and to contributions from numerous collaborators. Properties of biological aggregations. Large-scale coordinated movement No centralized control

343 views • 25 slides

Reduction of Particle and Heat Transport in HSX with Quasisymmetry

Reduction of Particle and Heat Transport in HSX with Quasisymmetry. J.M. Canik , D.T.Anderson, F.S.B. Anderson, K.M. Likin, J.N. Talmadge, K. Zhai HSX Plasma Laboratory, University of Wisconsin-Madison, USA. Outline.

277 views • 21 slides

Determining of Radial Profile of Hydrogen Isotope Composition of TCV plasmas

Determining of Radial Profile of Hydrogen Isotope Composition of TCV plasmas A.Karpushov, B.P.Duval, Ch.Schlatter, H.Weisen with contribution from Laboratory of Atomic Collision Physics, Ioffe PTI for 32 nd EPS Conference on Plasma Physics, 27 June - 1 July 2005 , Tarragona, Spain.

333 views • 20 slides

Standard Solar Model Calculation of Neutrino Fluxes

256 views • 17 slides

Peaked Density Profiles in Low Collisionality H-modes in JET, ASDEX Upgrade and TCV

Peaked Density Profiles in Low Collisionality H-modes in JET, ASDEX Upgrade and TCV. TCV.

215 views • 16 slides

Density profile changes are the result of the profile consistency effect. K.Razumova

Density profile changes are the result of the profile consistency effect. K.Razumova.

263 views • 15 slides

Size Selectivity in Ion channels

Size Selectivity in Ion channels. Roland Roth Dirk Gillespie. Model of Size Selectivity. what is the simplest system that shows the effect of size selectivity? mixture of uncharged hard spheres that model e.g. water, Na and K

286 views • 15 slides

Inflation + ?CDM Model = Cosmology Galaxies Formation

271 views • 14 slides

Field line tracing And 3D scrape-off density profiles

256 views • 13 slides

Density peaking in gyrokinetic simulations of H-mode plasmas in Alcator C-Mod

Density peaking in gyrokinetic simulations of H-mode plasmas in Alcator C-Mod. D. R. Mikkelsen, M. Bitter, K. Hill, PPPL M. Greenwald, A. Ince-Cushman, J. Rice, MIT J. Candy, R. Waltz, General Atomics ITPA Transport & Confinement Topical Group Workshop Milan, 20-22 October 2008.

255 views • 13 slides

185 views • 9 slides

Shock waves in cold Fermi atoms Alexander G. Abanov , Stony Brook University, DMR 0906866

Shock waves in cold Fermi atoms Alexander G. Abanov , Stony Brook University, DMR 0906866. We considered the collision of two clouds of ultracold Fermi atoms of 6 Li in elongated magnetic trap. Interactions between Li atoms were magnetically tuned to extremely strong ones.

211 views • 2 slides

Introduction :

Introduction :

81 views • 1 slides

Chemical and Physical Structures of Massive Star Forming Regions

Gas Temperature. Thermal Equilibrium G +L- L = 0 -> T gas (r). G : photoelectric heating on dust by FUV L : heating & cooling by collision between gas and dust particles L : cooling by line excitations. Chemical and Physical Structures of Massive Star Forming Regions.

120 views • 1 slides