'Reverse shock' presentation slideshows

Claes Fransson, Stockholm University

1.41k views • 120 slides

Cosmic Explosions in the Universe

Cosmic Explosions in the Universe. Poonam Chandra Royal Military College of Canada. Page # 1. Poonam Chandra. 13 th Sept 2011. Universe is 14 billion years old. Our sun is 5 billion years old. Supernovae and Gamma ray bursts explosions lasting fraction of a second to few seconds.

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Nonthermal Radiation from Merging Clusters of Galaxies

Nonthermal Radiation from Merging Clusters of Galaxies. Robert C. Berrington (NRL) Chuck Dermer (NRL) Penn State U., May 27 th , 2003. (ApJ, in press, 2003, astro/ph 0209436). Outline. Shocks are formed during structure formation in merging clusters of galaxies

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Collaborators

Models for early afterglows (shallow decay & X-ray flares) and implications for progenitors Zigao Dai Nanjing University 2008 Nanjing GRB Conference. Collaborators. Tan Lu, Daming Wei, Yongfeng Huang, Xiangyu Wang ? Nanjing GRB group, K. S. Cheng

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High Energy Astrophysics

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Circumstellar interaction in Type II SNe Evidence for CSI in different Type II SNe.

Circumstellar interaction in Type II SNe Evidence for CSI in different Type II SNe. CSI as a shock physics lab The ring collision of SN 1987A. How does it fit in?. SN 1993J. Radio: Synchrotron spectrum Wavelength dependent turn-on of emission VLBI imaging of SN 1993J and SN 1986J.

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Gamma-Ray Burst Early Afterglows

Gamma-Ray Burst Early Afterglows. Bing Zhang Physics Department University of Nevada, Las Vegas Dec. 11, 2005, Chicago, IL. Collaborators. E. W. Liang, Y. Z. Fan, J. Dyks & D. Proga (UNLV) S. Kobayashi (Livermore JMU) & P. Meszaros (PSU)

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Gamma-Ray Bursts Early Afterglows

Gamma-Ray Bursts Early Afterglows. Bing Zhang Physics Department University of Nevada, Las Vegas Jun. 21, 2005, Torun, Poland. Collaborators. S. Kobayashi (PSU) P. Meszaros (PSU) Y. Z. Fan (UNLV & PMO) D. M. Wei (PMO) J. Dyks (UNLV & NCAC)

552 views • 41 slides

Pulsar Wind Nebulae

Pulsar Wind Nebulae. http://www.astroscu.unam.mx/neutrones/home.html. Rotating magnetosphere generates E X B wind - direct particle acceleration as well, yielding (e.g. Michel 1969; Cheng, Ho, & Ruderman 1986). The Pulsar Wind Zone. Magnetic polarity in

493 views • 30 slides

Supernova Remnants

Supernova Remnants. and GLAST. Reverse Shock. PWN Shock. Forward Shock. Pulsar Termination Shock. Pulsar Wind. Unshocked Ejecta. Shocked Ejecta. Shocked ISM. PWN. ISM. SNRs: The (very) Basic Structure. Pulsar Wind - sweeps up ejecta; shock decelerates

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Cosmic-ray acceleration in radio supernovae

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Pulsar Wind Nebulae

Observations of. Pulsar Wind Nebulae. Jet/Torus Structure in PWNe. Anisotropic flux with maximum energy flux in equatorial zone - radial particle outflow - striped wind from Poynting flux decreases away from equator Wind termination shock is farther from

343 views • 20 slides

Dust in SNR 1E 0102.2?7219

Dust in SNR 1E 0102.2?7219. Karin M. Sandstrom et al. 2009. Dust, a crucial component. for interstellar chemistry regulates thermal balance A Shield for dense clouds. Mid-IR emission from Newly Formed Dust. ? 400 and 800 days after the explosion

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Gamma-Ray Burst models Theory of prompt and afterglow emission

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Taking a Broad View of Prompt Emission

Taking a Broad View of Prompt Emission. Contemporaneous emission at eV and ~0.1 MeV. Sarah Yost, for the ROTSE Collaboration Venice, June 2006. Key Points. prompt : contemporaneous with ? -rays importance of broadband view prompt less understood synchrotron emission? afterglow onset

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Observations of Pulsar Bowshock Nebulae

Observations of Pulsar Bowshock Nebulae. Collaborators: B. M. Gaensler T. Temim J. D. Gelfand E. van der Swaluw S. Chatterjee. Bow Shock PWNe: Introduction. Formed by supersonic motion of pulsar through surrounding medium - can occur within host SNR or in ISM

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Multi-wavelength Observations of Composite Supernova Remnants

Multi-wavelength Observations of Composite Supernova Remnants. Collaborators: Patrick Slane (CfA) Eli Dwek (GSFC) George Sonneborn (GSFC) Richard Arendt (GSFC) Yosi Gelfand ( NYU Abu Dhabi) Paul Plucinsky (CfA) Daniel Castro (MIT). Tea Temim (NASA GSFC/ORAU).

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(relativistic) magneto-hydrodynamics of plerions basic paradigm and issues

216 views • 8 slides