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There are two possible outcomes when a star uses up its helium or other elements, depending on its mass.
1. Low-mass stars (up to about 8 times the mass of our Sun):
Once a low-mass star exhausts its helium fuel in the core, it does not have sufficient mass or pressure to ignite fusion of heavier elements, like carbon or oxygen. The core then contracts due to gravity, while the outer layers of the star expand, forming a red giant. Eventually, the star sheds its outer layers, leaving behind a dense, hot core called a white dwarf. This core is composed mostly of carbon and oxygen, and it is supported against gravity by electron degeneracy pressure. Over time, the white dwarf cools down and becomes a dim, compact object, known as a black dwarf.
2. High-mass stars (more than about 8 times the mass of our Sun):
When a high-mass star consumes the helium in its core, fusion reactions to create heavier elements continue. The star undergoes multiple fusion stages wherein it fuses heavier and heavier elements, ultimately forming iron in its core. However, fusion of iron is not energetically favorable, so the core cannot sustain itself against gravity. The core collapses under its own weight very rapidly, leading to a cataclysmic event known as a supernova. During a supernova explosion, the outer layers of the star are ejected into space while the core collapses further. Depending on the mass of the core, it can result in the formation of either a neutron star or a black hole.
In summary, low-mass stars end their lives as white dwarfs, while high-mass stars end their lives in supernova explosions, forming either neutron stars or black holes.
When a star uses up its helium or other elements, it collapses inwards due to the force of gravity. The specific process that occurs depends on the mass of the star.
For lower mass stars, such as our Sun, after using up its helium, it enters a phase called the red giant phase. During this phase, the star expands and its outer layers become less dense, causing it to cool down and appear redder. Eventually, the outer layers of the star are expelled into space, leaving behind a dense core known as a white dwarf. This core is made up of mostly carbon and oxygen and is about the size of the Earth.
In the case of more massive stars, the collapse after using up their helium is much more dramatic. These stars undergo a supernova explosion. As the core of the star collapses, it rebounds outward, triggering a massive explosion that can outshine an entire galaxy. This explosion disperses heavy elements into space and leaves behind a neutron star or, if the mass is large enough, a black hole.
In summary, when a star uses up its helium or other elements, it can either form a white dwarf in the case of lower mass stars or undergo a supernova explosion followed by the formation of a neutron star or black hole, depending on its mass.
When a star uses up its helium or other elements, it undergoes a process called stellar collapse. This collapse can lead to different outcomes depending on the mass of the star.
For stars with a lower mass, less than about 1.4 times the mass of our Sun, the collapse results in the formation of a white dwarf. A white dwarf is a dense, hot stellar remnant composed mainly of carbon and oxygen. The core of the star collapses while its outer layers are expelled through a planetary nebula, leaving behind the highly compressed, glowing core.
On the other hand, for more massive stars, the collapse can lead to a much more dramatic event known as a supernova. As the core of the star runs out of fuel, it is unable to support itself against gravity. The core rapidly collapses under its own gravitational pull, resulting in an enormous release of energy. This explosion is known as a supernova, which can outshine entire galaxies for a brief period of time.
In the most extreme cases, the core collapse might not be halted by the explosion, causing the formation of a black hole. This occurs when the core collapses into an infinitesimally small, infinitely dense point called a singularity, surrounded by an event horizon from which nothing, not even light, can escape.
To determine the fate of a collapsing star, scientists use a combination of observations and theoretical models. They study the behavior of stars throughout their lives, from birth to death, and analyze various factors such as mass, composition, and evolutionary stage to predict the outcomes. Additionally, the study of supernovae and the remnants they leave behind helps refine our understanding of stellar collapse and its aftermath.