Introduction to Stars

What's on This Page


What are Stars?

A star is a dense mass that generates its light and heat by nuclear reactions, specifically by the fusion of hydrogen and helium under conditions of enormous temperature and density. When the hydrogen atom merges with the next heavier element, helium, mass is lost, thus the mass is converted to hydrogen (E=mc^2). The sun, which is our closest star, is powered by hydrogen fusion. The fusion only takes place at core of the star where it is dense enough.

How does X-ray Astronomy Fit In?

Most stars emit X-rays which satellites can detect. These X-ray images look very different from what we see with our eyes. They show us the hotter areas of gas surrounding stars (stellar coronae), the hottest stars (young white dwarfs), and flares from stars.

X-ray image of IC 348
optical image of IC 348
X-ray imageOptical image
ROSAT (X-ray) and optical images of the central 20 arcmin region of IC 348, a young star cluster. Notice the differences in the brightness of these stars in optical and X-ray light.

Further Star Resources and References



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Last modified: Thursday, 26-Jun-2003 13:48:45 EDT