'Slow wind' diaporamas de présentation

NSO Summer School Lecture 2: Solar Wind Turbulence

NSO Summer School Lecture 2: Solar Wind Turbulence. Charles W. Smith Space Science Center University of New Hampshire Charles.Smith@unh.edu. Good References (Still):.

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Turbulence and Intermittency in the Solar Wind

Turbulence and Intermittency in the Solar Wind. R. Bruno 1 In collaboration with : 3 Carbone, V., 1 Bavassano, B., 1 D'Amicis, R., 4 Sorriso, L., 5 Pietropaolo, E 1 Istituto di Fisca dello Spazio Interplanetario, INAF, Rome , Italy

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Axisymmetrical velocity structure in bipolar PNe

Axisymmetrical velocity structure in bipolar PNe. Martina Dobrin ? i ?. M. Guerrero, A. Manchado, E. Villaver. Introduction. The mechanism (s) responsible for shaping of a wide range of bipolar objects are still poorly understood

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A Whole-Heliosphere View of the Solar Wind Hale Lecture American Astronomical Society 5/24/2010

A Whole-Heliosphere View of the Solar Wind Hale Lecture American Astronomical Society 5/24/2010. Marcia Neugebauer University of Arizona. The Things that Happen to the Solar Wind After it Leaves the Sun. A Better Title:. The Complex Solar Atmosphere.

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A Whole-Heliosphere View of the Solar Wind Hale Lecture American Astronomical Society 5/24/2010

A Whole-Heliosphere View of the Solar Wind Hale Lecture American Astronomical Society 5/24/2010. Marcia Neugebauer University of Arizona. The Things that Happen to the Solar Wind After it Leaves the Sun. A Better Title:. The Complex Solar Atmosphere.

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Tracing Heliospheric Structures to Their Solar Origin Robert Wimmer-Schweingruber

Tracing Heliospheric Structures to Their Solar Origin Robert Wimmer-Schweingruber wimmer@physik.uni-kiel.de Christian Albrechts University Kiel Kiel, Germany for the Solar Orbiter Team. Tracing Heliospheric Structures to Their Solar Origin The Problem What can we measure? Linkage...

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At a loss for words?

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The Effect of Solar Wind on Pulsar Observations

The Effect of Solar Wind on Pulsar Observations. Xiaopeng YOU Southwest University, Chongqing, China. Outline. Introduction Our solar wind model Solar wind effect 1: DM variations Solar wind effect 2: RM variations Conclusion. Introduction ---motivation. Main goal of PPTA project

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Solar Wind Transients and SEPs

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Physics of Relativistic Jets

Physics of Relativistic Jets. Yuri Lyubarsky. Ben-Gurion University Beer- Sheva , Israel . Universality of relativistic jets. M 87. M 87. Crab in X-rays. t ime, s. t ime, s. PKS 2155-304 . GRBs.

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Abundances in the Solar Atmosphere and in the Solar Wind

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Helium Variation Across Two Solar Cycles Reveals A Speed-Dependent Phase Lag

Helium Variation Across Two Solar Cycles Reveals A Speed-Dependent Phase Lag. B. L. Alterman & Justin C. Kasper July 18, 2019. Solar Wind Helium Abundance & Sunspot Number (SSN). Definitions. Published Observations. Strongest in slow wind ( Falls off for Helium vanishing speed

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CME Propagation

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Signatures of Time-dependent Heating in Active Regions and the Slow Solar Wind

Signatures of Time-dependent Heating in Active Regions and the Slow Solar Wind. Organizers : Steve Bradshaw, Will Barnes ( Rice University); Nicki Viall ( GSFC). Scene setting speakers :

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