It is the band on the H-R diagram in which stars are arranged as they begin their extended period of stable nuclear fusion.

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What happens to the surface temperature and radius of a star like the Sun as it goes from the main sequence to the red giant branch?
They contain from hundreds of thousands to millions of stars and have a typical size of about 50 parsecs.
While a star is on the main sequence, its equilibrium is the result of the outward pressure of hot gas and the inward pressure of ________.
A white dwarf in a binary system suddenly flares, but in a few months it settles back to its original luminosity. This process may repeat many times. What object is it?
The reflection nebula is a cloud of dust. When light from a star encounters this cloud, the short wavelength blue light "bounces back" from the cloud towards us, and the longer wavelength red light passes through.
Enough material is drawn onto a white dwarf to increase its mass to the point of collapse, and all of its material fuses at once.
Type I supernovae occur only in binary or other multiple-star systems, whereas Type II supernovae occur in isolated single, high-mass stars.
Which of the following is the best description of the interior structure of a highly evolved high-mass star late in its lifetime but before the collapse of its iron core?
An onion-like set of layers forms, with the heaviest elements in the innermost shells surrounded by progressively lighter ones.
The stars in any particular cluster formed at roughly the same time from the same primary material and under the same environmental conditions.

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Which of the following statements is true for the Hertzsprung-Russell diagram of an isolated star cluster approximately 1 billion years old?
It would be depleted of O- and B-type stars from the main sequence, with all other stars occupying the main sequence except for a few white dwarfs.
As a low-mass main-sequence star runs out of fuel in its core, it actually becomes brighter. How is this possible?
Which of the following best describes what happens to a one-solar-mass star when it reaches the main sequence?
What is the key factor that determines the temperature, density, radius, luminosity, and pace of evolution for a prestellar object?
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