A high-mass star will use up its fuel faster than a low-mass one. Depending on the amount of mass that remains at the end of its life, it may convert to a neutron star, or to a black hole.
The stage that comes first in the life cycle of a high-mass star is the main sequence stage. During this stage, the star fuses hydrogen into helium in its core, maintaining a balance between radiation pressure and gravity.
The more the mass the shorter their life cycle (the more quickly they use their fuel)
The Sun is a medium mass star in main sequence.
its mass
high mass has shortest life (stars right?)
The key element that indicates a star is living a high mass life cycle is the presence of heavier elements such as carbon, oxygen, and eventually iron in its core. High mass stars undergo fusion processes that produce these heavier elements during their relatively short lifetimes. In contrast, low mass stars primarily fuse hydrogen into helium and may only produce lighter elements before they evolve into red giants and shed their outer layers, leaving behind white dwarfs. The ability to create and sustain fusion of heavier elements is a hallmark of high mass star evolution.
mass
Two similarities in the life cycle of high-mass stars include the stages of nuclear fusion and the eventual formation of supernovae. Both high-mass stars undergo a series of fusion processes, starting with hydrogen and progressing to heavier elements like helium, carbon, and iron. Ultimately, when they can no longer support fusion, these stars explode as supernovae, leading to the formation of neutron stars or black holes. Additionally, both types of high-mass stars experience significant mass loss through stellar winds throughout their lives.
The life cycle of a star is determined primarily by its mass. The hotter a star the bluer its color. The difference between apparent brightness and luminosity is that luminosity is a good indicator of the energy output of a star.
A star's "life cycle" depends mostly on its initial mass; everything is determined by mass. Small, low-mass stars may shine essentially forever, while very large high-mass stars may grow old and go supernova in only a few dozen million years.
The more massive a star is, the less its life time.
At the end of its life cycle, a high mass star can leave behind either a neutron star or a black hole. If the remaining core has a mass between about 1.4 and 3 solar masses, it typically collapses into a neutron star, which is incredibly dense and composed mostly of neutrons. If the core's mass exceeds approximately 3 solar masses, it collapses further into a black hole, where gravity is so strong that not even light can escape its grasp.