'Coronal mass ejections' presentation slideshows

Guiding Questions

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The American Geophysical Union Space Physics and Aeronomy Section

FROM SUN TO EARTH. The American Geophysical Union Space Physics and Aeronomy Section. The American Geophysical Union (AGU) Space Physics and Aeronomy (SPA) Section.

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Space Science and the Engines of Change

Space Science and the Engines of Change. Keith Mason CEO UK Science & Technology Facilities Council. Astronomy as a change engine. Human kind is instinctively curious about the world and their place in it Astronomy, the oldest science, is accessible to all

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THE SUN

THE SUN. The star we see by day. Goals. Summarize the overall properties of the Sun. What are the different parts of the Sun? Where does the light we see come from? The scientific method: solar neutrinos. The Sun, Our Star. The Sun is an average star.

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Our Sun

Our Sun. A medium sized star. Our Sun. Our sun is a typical medium sized star. A star is a hot ball of plasma that shines because nuclear fusion is taking place at its core It is composed of 73% hydrogen, 25% helium and 2% of other elements such as carbon, oxygen and iron.

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Coronal Prominence Cavities: Magnetism and Dynamics

Coronal Prominence Cavities: Magnetism and Dynamics. Sarah Gibson, Giuliana de Toma , Therese Kucera , Kathy Reeves, Donald Schmit , and Alphonse Sterling. Abstract.

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The Sun, our favorite star!

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Our Star, the Sun

Our Star, the Sun. The Sun is the Largest Object in the Solar System. The Sun contains more than 99.85% of the total mass of the solar system If you put all the planets in the solar system, they would not fill up the volume of the Sun

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ASTRONOMY

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The Sun

The Sun. The Sun. 70% hydrogen and 28% helium. Is a star Made of gases Is our primary source of energy Contains 99.8% of the entire mass of Solar System. Light (radiation). Image at http://science.nasa.gov/headlines/y2007/images/chromosphere/LimbFlareJan12_strip2.jpg.

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An Introduction to Space Weather

COSMO K-Coronagraph Science Requirement s. An Introduction to Space Weather. Joan Burkepile. J. Burkepile High Altitude Observatory / NCAR. http://www.cosmo.ucar.edu/kcoronagraph.html. Science Goals.

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The Sun

Visual (photosphere). The Sun. UV (chromosphere). (1) Basic Properties. Rotates once per month. Big : R sun ~ 100 R earth Massive : M sun ~ 3 x 10 5 M earth Ave. Density = Mass/Volume < ? sun > = 1.4 gm/cm 3 (~ ? water )

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Understanding Sunspots

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Radio Meteor Detection at the NLO

Radio Meteor Detection at the NLO. by Andy Smith G7IZU. This PowerPoint presentation will play automatically in a few seconds. v.1.0 2010-07-28. Meteors can be detected by receiving radio signals reflected from their trails. What do we need to detect meteors?.

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Grades 3 - 5: Introduction

Grades 3 - 5: Introduction. Sun-Earth Connection:. Our Star - Our Sun. Importance of Space Technology. Better Observation Of The Sun And Earth. Solar Sails and Space Exploration. Structure Of The Sun. Inside The Sun. Sunspots. Solar Flares. Coronal Mass Ejections.

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Grades 3 - 5: Introduction

Grades 3 - 5: Introduction. Sun-Earth Connection:. Our Star - Our Sun. Importance of Space Technology. Better Observation Of The Sun And Earth. Solar Sails and Space Exploration. Structure Of The Sun. Inside The Sun. Sunspots. Solar Flares. Coronal Mass Ejections.

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Coronal Mass Ejections without photospheric / chromospheric signatures

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Spectroscopic Diagnostics and Imaging of SEP Production in Current Sheets and CME Shocks

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