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There are two main forces acting in a star: Gravitational contraction: it is due to the higher layers, this force pushes mass to the center. Radiation pressure: it is produced by the inner layers, and it forces material upwards.
Once a medium size star (such as our Sun) has reached the red giant phase, its outer layers continue to expand, the core contracts inward, and helium atoms in the core fuse together to form carbon.
A star’s life is all about trying to maintain hydrostatic equilibrium, or a balance between the force of gravity trying to contract the star and the pressure generated by the heat released in nuclear fusion in the star’s interior.
stars. These black holes pack in about four to a few tens of solar masses. To understand how such black holes can form, let us briefly review the life cycle of a massive star. For stars some 7 or more times as massive as our Sun, fate has something very special in store when they begin to run out of hydrogen to fuse into helium.
In this class, we will define four fundamental equations of stellar structure, and several additional relationships that, taken all together, will define the structure of a star and how it evolves with time.
Lesson Objectives and Overview: Stars explores the various types of stars in the universe and their lifecycle. Students will discover how scientists categorize and classify the universe’s suns and define certain smaller groups into constellations.
What is a star? Why do they shine and seem to twinkle? Where do stars come from? What is a constellation? Why did people name patterns of stars and create stories about them? Books and activities. Books: fiction, nonfiction and poetry all about stars, constellations, and comets.
