'Stellar wind' diaporamas de présentation

An Astrophysical Counter-Paradigm: * The Hubble Treasury Project for Eta Carinae

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Astro 201: Oct. 5, 2010

Astro 201: Oct. 5, 2010. Today : The Evolution of the Sun The Evolution of Massive Stars Origin of the Elements White Dwarfs, Neutron Stars, Black Holes. Illustrations from Prof. Terry Herter's web site and Prof. Richard Pogge's web site. 1. Protostar Phase (50 million years)

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Lecture 9: More About Extrasolar Planets

Lecture 9: More About Extrasolar Planets. Predicted weather patterns on HD80606. Please remind me to take a break at 12:45 pm!. Claire Max May 1, 2014 Astro 18: Planets and Planetary Systems UC Santa Cruz. Page . Outline of lecture. Formation of protoplanetary disks

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X-Ray Astronomy and Accretion Phenomena

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The Rocket Science of Launching Stellar Disks

The Rocket Science of Launching Stellar Disks. Stan Owocki UD Bartol Research Institute. Stan Owocki Bartol Research Institute University of Delaware. Disks in Space. Where do stars, planets, we, come from??. From collapse of interstellar gas clouds Gravity pulls together

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Recent results from the SIMECA code and the VLTI observations

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Solar/Stellar Winds: An Overview

Solar/Stellar Winds: An Overview. (Untapped gold mines for space physicists?). Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics. Outline. The Stellar Zoo:. The Sun Young low-mass stars (T Tauri, FU Ori, etc.) Evolved low-mass stars (giants, supergiants, Miras)

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The Deaths of Stars

0. Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). 0. The Deaths of Stars. Chapter 13. 0. Guidepost.

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The Deaths of Stars

0. The Deaths of Stars. Chapter 13. 0. Guidepost.

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Links Between Pulsations & Line-Driven Mass Loss in Massive Stars

Possible. Links Between Pulsations & Line-Driven Mass Loss in Massive Stars. Stan Owocki Bartol Research Institute University of Delaware. IAU Colloquium #185 Leuven, Belgium July 26-31, 2001. Outline. Key properties of line-driven mass loss Wind variability

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Orbital evolution of compact Black-hole binaries and white dwarf binaries

Orbital evolution of compact Black-hole binaries and white dwarf binaries. Astro-ph/0511760. Astro-ph/0510331. Wencong Chen. Astro-ph/0511760. Magnetic braking of Ap/Bp stars: application to compact BH X-ray binaries. 1.Introduction:. Conventional magnetic braking (MB):.

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Nature of X-ray binaries in the Magellanic Clouds

Nature of X-ray binaries in the Magellanic Clouds. Andry RAJOELIMANANA 1 , 2 ( MSc ) Supervisor : Prof Phil CHARLES 1 , 2. 1 University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa.

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Asymptotic Giant Branch Stars

Asymptotic Giant Branch Stars. Ashley Nord December 3, 2007. What are Asymptotoic Giant Branch (AGB) Stars?. Stars with masses ? 8M on the second ascent into the Red Giant Region Often AGBs are Long-Period Variables

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Asymptotic Giant Branch Stars

Asymptotic Giant Branch Stars. Ashley Nord December 3, 2007. What are Asymptotoic Giant Branch (AGB) Stars?. Stars with masses ? 8M on the second ascent into the Red Giant Region Often AGBs are Long-Period Variables

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The Application of Forbidden Line X-Ray Diagnostics to the Hot Star Tau Sco

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Acceleration of GCR in stellar winds and the GCR 22 Ne/ 20 Ne source ratio N. Prantzos

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The dynamics of microquasar jets in HMXBs

The dynamics of microquasar jets in HMXBs. Relativity meeting 2013.10.27 DooSoo Yoon UW-Madison s upervised by Prof. Heinz. Interaction w/ medium. M87, Virgo cluster (Hubble WFPC2). Cygnus X-1 (Gallo 2005). Interaction w/ medium. Adavantage to study X-ray Binaries

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Windsock memory conditioned ram pressure effect: forced magnetic reconnection

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