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A star topology uses a central network device, such as a hub or a switch, to connect all nodes in the network. Each node is connected directly to the central device, creating a centralized architecture that simplifies network management and troubleshooting.
Because a massive star has more pressure on the core, this creates greater temperatures, which increase the amount of nuclear fusion that occurs. This uses more hydrogen and thus the star runs out of fuel much quicker, that a smaller star.
This happens when a main sequence star uses up all of its fuel and swells. Next stage: Red Giant.
Right now the sun is a main sequence star. When it uses up the hydrogen in its core it will become a red giant then shed its outer layers to become a white dwarf.
The lifetime of a massive star is shorter than that of a star like the sun. Massive stars have more fuel to burn but burn it at a faster rate due to their higher core temperatures and luminosities. This leads to a shorter lifespan for massive stars compared to sun-like stars.
The major difference is that a low-mass star lives much longer. The reason for this is that a high-mass star gets hotter, is much brighter, and uses up its fuel much faster. The difference can be quite dramatic, with some stars being millions of times brighter than others. Also, assuming the star doesn't acquire additional mass, a low-mass star will end up as a white dwarf, while more massive stars will end up as a neutron star, or in the case of the most massive stars, a black hole.