'Number density' diaporamas de présentation

Introduction to the Physics of Saturation

Introduction to the Physics of Saturation. Yuri Kovchegov The Ohio State University. Outline. General concepts Classical gluon fields, parton saturation Quantum (small-x) evolution Linear BFKL evolution Non-linear BK and JIMWLK evolution Recent progress (selected topics)

1.2k views • 104 slides

Introduction to the Physics of Saturation

Introduction to the Physics of Saturation. Yuri Kovchegov The Ohio State University. Outline. Preamble Review of saturation physics/CGC. Classical fields Quantum evolution More recent progress at small-x Running coupling corrections NLO BFKL/BK/JIMWLK corrections Conclusions.

656 views • 57 slides

651 views • 52 slides

S. Shibata ?? ??? Yamagata Univ. ???? Department of Phys ????

? FAN3 22 June 2012. The Structure of the Pulsar Magnetosphere via Particle Simulation. S. Shibata ?? ??? Yamagata Univ. ???? Department of Phys ????. Aim of our numerical study. via particle simulation, the main problems to be challenged are.

640 views • 50 slides

Selected literatures introduction about gas-liquid flow in microchannels

Selected literatures introduction about gas-liquid flow in microchannels. Reporter: Zhang Weihua Supervisor: Professor Xin Feng. Contents. Fundamentals. Flow patterns Mixer geometry Pressure drop. Fundamentals. Flow patterns.

608 views • 40 slides

Yuk Yung, Peter Gao , Xi Zhang, David Crisp, and Charles G. Bardeen DPS 44 October 17 th , 2012

Generation of Aerosol Particles via Nucleation of Meteoric Dust and Cloud Upwelling in the Upper Haze of Venus. Yuk Yung, Peter Gao , Xi Zhang, David Crisp, and Charles G. Bardeen DPS 44 October 17 th , 2012. Observations: The Upper Haze is variable on the order of days .

494 views • 38 slides

Progress Towards Developing a Self-Consistent Model for the Production and Transport of SEPs by CME-Driven Shocks

601 views • 31 slides

422 views • 31 slides

21cmFAST A Fast, Semi-Numerical Simulation of the High-Redshift 21cm Signal

21cmFAST A Fast, Semi-Numerical Simulation of the High-Redshift 21cm Signal. Mesinger, Furlanetto , & Cen (2010). Andrei Mesinger Princeton University. Motivation. We know next to nothing about high-z --> ENORMOUS parameter space to explore

656 views • 29 slides

1. MEASURES OF ATMOSPHERIC COMPOSITION

1. MEASURES OF ATMOSPHERIC COMPOSITION. WHAT IS THE ATMOSPHERE?. Gaesous envelope surrounding the Earth Mixture of gases, also contains suspended solid and liquid particles ( aerosols) Aerosol = dispersed condensed phase suspended in a gas.

415 views • 23 slides

Holographic QCD in the medium

Holographic QCD in the medium . Chanyong Park ( CQUeST ) @ LHC Physics Workshop (2010.08.11). Ref. B. H. Lee, CP and S.J. Sin, JHEP 0907 (2009) 087. CP, Phys. Rev. D81, (2010) 045009. K. Jo, B. H. Lee, CP and S.J. Sin, JHEP 1006 (2010) 022. 1. AdS /CFT correspondence

370 views • 22 slides

The rate of expansion of Universe

The rate of expansion of Universe. Consider a sphere of radius r=R(t) ? , If energy density inside is ? c 2 ? Total effective mass inside is M = 4 ?? r 3 /3 Consider a test mass m on this expanding sphere, For Test mass its Kin.Energy + Pot.E. = const E

299 views • 19 slides

QUESTIONS

395 views • 18 slides

326 views • 17 slides

Buffer Gas Cooling of atomic and molecular beams

Wenhan Zhu Princeton University 11/06/2007. Buffer Gas Cooling of atomic and molecular beams. Basic idea. The technique relies on thermalization of the species-to-be-trapped via collisions with a cold buffer gas, which serves to dissipate the translational energy of the atoms or molecules.

361 views • 16 slides

Weak lensing of CMB from cosmic (super-)strings

9/28/2011 JGRG21 @ Tohoku U. Weak lensing of CMB from cosmic (super-)strings. Daisuke Yamauchi. ICRR, U Tokyo. w ith A. Taruya (U Tokyo, RESCEU), T. Namikawa (U Tokyo), K. Takahashi (Kumamoto U), Y. Sendouda ( Hirosaki U) , C.M. Yoo (YITP). Introduction. CMB lensing .

364 views • 15 slides

Lecture 6

Lecture 6. The radiation field and opacity. Review. The main sequence is a mass sequence More massive stars are closer to the top-left (hot and bright). M=30M Sun. M=M Sun. M=0.2M Sun. Radiation intensity.

407 views • 14 slides

Update on MISR applications to Shrub Abundance Mapping in Desert Grasslands

Update on MISR applications to Shrub Abundance Mapping in Desert Grasslands. Mark Chopping, Lihong Su, Albert Rango, Debra P.C. Peters, John V. Martonchik, and Andrea Laliberte 3 March 2006. Structure: A Strength of Multiangle Remote Sensing .

171 views • 7 slides

Lecture 8: Div(ergence)

Lecture 8: Div(ergence). Consider vector field and. outside. Flux (c.f. fluid flow of Lecture 6) of out of S . inside. e.g, if is the fluid velocity (in m s -1 ), . S. rate of flow of material (in kg s -1 ) out of S

170 views • 7 slides

3.2 Spatial distribution differences

A Comparison of Extratropical Cyclones in Recent Reanalyses. 1 Introduction

118 views • 1 slides