Main Sequence Star

The newly formed star continues to contract for about another 30 million years after nuclear fusion has begun; the central density increases to 1032 particles per cubic meter, the central temperatures rise to 15,000,000 K, and the surface heats to about 6,000 K. At this stage the thermal pressures balance the gravitational contraction forces, and the rate that nuclear energy is generated in the core equals that at which it is radiated at the surface. At this stage the star has reached the main sequence, where it can burn stably for about another 10 billion years without significantly changing.

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How To Survive The End Of The World

How To Survive The End Of The World

Preparing for Armageddon, Natural Disasters, Nuclear Strikes, the Zombie Apocalypse, and Every Other Threat to Human Life on Earth. Most of us have thought about how we would handle various types of scenarios that could signal the end of the world. There are plenty of movies on the subject, psychological papers, and even survivalists that are part of reality TV shows. Perhaps you have had dreams about being one of the few left and what you would do in order to survive.

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