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.
Continue reading here: Variations In Stellar Formation With Solar Mass
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