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4. Shock

4. Shock

4. Shock. Outline:. Introduction of the shock. The shock in the space. The property of the shock. Why do we want to study shock? Shock acceleration of the particles. Bow Shock CIR shock and Interplanetary traveling shock Termination shock and Anomalous Cosmic ray. What is a shock?.

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2.43k views • 72 slides
Motivation

Motivation

What is Role of Proton Beams in Solar Radio Bursts? Jun-ichi Sakai Laboratory for Plasma Astrophysics University of Toyama, Japan. Motivation.

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506 views • 45 slides
Non-neutral Plasma Shock

Non-neutral Plasma Shock

Non-neutral Plasma Shock. ? HU Xiwei ????? HE Yong ???? Hu Yemin ????? Huazhong University of Science and Techonology 2006.10.25 Zhejiang University, Hangzhou, China. Outline. Introduction Motivation One dimensional case

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549 views • 39 slides
Supernovae

Supernovae

Supernovae. High Energy Astrophysics emp@mssl.ucl.ac.uk http://www.mssl.ucl.ac.uk/. Introduction. Supernovae occur at the end of the evolutionary history of stars. The star must be at least 2 solar masses: the core at least 1.4 solar masses.

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554 views • 38 slides
Scales at High Mach Number Quasiperpendicular Shocks and Problem of Electron Heating

Scales at High Mach Number Quasiperpendicular Shocks and Problem of Electron Heating

Scales at High Mach Number Quasiperpendicular Shocks and Problem of Electron Heating. Vladimir KRASNOSELSKIKH LPC2E / CNRS-University of Orleans S.J. Schwartz, D. Sundqvist, F. Mozer. Electron Heating Scale at High Mach Number Quasiperpendicular Shocks. Plan Introduction

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480 views • 38 slides
Colliding winds in pulsar binaries

Colliding winds in pulsar binaries

Colliding winds in pulsar binaries. S.V.Bogovalov 1 , A.V.Koldoba 2 ,G.V.Ustugova 2 , D. Khangulyan 3 , F.Aharonian 3 1-National Nuclear Research University (Moscow) 2-Institute of applied mathematics RAN (Moscow) 3-Max-Planck-Institute for Nuclear Physics (Heidelberg). Candidates.

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347 views • 25 slides
Feedback Effects of the First Stars on Nearby Halos

Feedback Effects of the First Stars on Nearby Halos

Feedback Effects of the First Stars on Nearby Halos. Kyungjin Ahn The University of Texas at Austin The End of the Dark Ages STSCI March 13 , 200 6. Outline. Introduction Code Description Initial Setup Result Conclusion. Dark Ages and Reionization.

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319 views • 22 slides
Accretion Processes in X-rays: From White Dwarfs to Quasars Boston, MA 14 July 2010

Accretion Processes in X-rays: From White Dwarfs to Quasars Boston, MA 14 July 2010

A New View of Accretion Shock Structure Nancy S. Brickhouse Harvard-Smithsonian Center for Astrophysics Collaborators: Steve Cranmer, Andrea Dupree, Juan Luna, and Scott Wolk. Accretion Processes in X-rays: From White Dwarfs to Quasars Boston, MA 14 July 2010.

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342 views • 19 slides
Charlie Jui ICAHTLT Sedona, AZ, Aug 10,1999

Charlie Jui ICAHTLT Sedona, AZ, Aug 10,1999

The Physics of Ultra-High Energy Cosmic Rays (UHECR) and Their Detection with Fluorescence Detectors. Charlie Jui ICAHTLT Sedona, AZ, Aug 10,1999. Outline. Introduction to Cosmic Rays Acceleration Mechanisms and Possible Sources Detection of Cosmic Rays

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327 views • 19 slides
Some open questions in the study of WDM/HEDM using laser driven shock

Some open questions in the study of WDM/HEDM using laser driven shock

Some open questions in the study of WDM/HEDM using laser driven shock. Andrew Ng University of British Columbia, Canada. IBD HEDP Workshop, Pleasanton, CA, June 22-24, 2010. Peter Celliers, UBC Luiz Da Silva, UBC Andrew Forsman, UBC Dean Parfeniuk, UBC Jim Waterman, UBC Guang Xu, UBC.

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330 views • 18 slides
Supernova Remnants

Supernova Remnants

Supernova Remnants. Shell-type versus Crab-like Phases of shell-type SNR. Shell-type SNR. Shell-type SNR: X-ray, radio, and optical emission come from a shell. X-rays are usually thermal, but can have non-thermal components. Shell is expanding.

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252 views • 15 slides
Supernova Remnants

Supernova Remnants

Supernova Remnants. Shell-type versus Crab-like Phases of shell-type SNR. Shell-type SNR. Shell-type SNR: X-ray, radio, and optical emission come from a shell. X-rays are usually thermal, but can have non-thermal components. Shell is expanding.

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164 views • 15 slides
Turbulence and Magnetic Field Amplification in the Supernova Remnants

Turbulence and Magnetic Field Amplification in the Supernova Remnants

Turbulence and Magnetic Field Amplification in the Supernova Remnants. TI, Yamasaki & Inutsuka (2009) in preparation. Tsuyoshi Inoue (NAOJ). Ryo Yamazaki (Hiroshima Univ.) Shu-ichiro Inutsuka (Kyoto Univ.). Introduction. Supernova r emunants ( SNRs ):

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293 views • 14 slides
Motivation

Motivation

6 ps. Shock-induced instabilities are hard to study by h ydrodynamic codes. l ~36 nm. h 0 (t=0)~36 nm. 2. 10.2 ps. 24.7 ps. Cu. vacuum. 29.2 ps. 36.3 ps. 1. 5. U pist =0.7. U pist =1.0. 15.7 ps. 25.9 ps. piston. 3. u p. h. u s. jetting. U p =1.0. U p =0.7. 42.6 ps.

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128 views • 1 slides

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