Slide 1

Facts about the Sun

The Sun is our star

Solar Observing in the Space Age

Names of things on the Sun

We probe the Sun’s interior using helioseismology

The patterns of resonating waves reveal the Sun’s interior structure and motions

The Doppler effect reveals ripples on the surface

The Sun rotates faster at its Equator than its Poles

Earlier helioseismology results: plasma rivers

Recent results: rotation is variable at all depths

Implications for magnetic fields: a dynamo

The deep origins of the Sun Earth connection

Magnetic fields observed on the solar surface

Magnetic fields control the Sun’s atmosphere

We see different parts of the Sun’s atmosphere by looking in different colors

The Sun’s corona is filled with magnetic loops

Sunspot activity follows an 11-year cycle

Comparing the Sun: 1996 to 1999

A Coronal Mass Ejection (CME)

CMEs busting out all over

How to recognize an Earth-bound CME

Sigmoids in the X-ray corona

S marks the spot animation

Space weather: a CME approaching Earth

Earth’s Magnetosphere and a CME

Earth’s magnetosphere reacting to a CME

Auroras often occur when a CME hits Earth

The auroral oval

CME impact on Earth’s magnetosphere

Aurora as seen from space

Powerful magnetic storm: 1989

When CMEs impact our magnetosphere

How can we prepare for CMEs?

Many related Web sites can be explored

Web sites about the Sun Earth Connection

Acknowledgements