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Class 12 Tuition > Learn Class XI-XII Tuition (PUC) > How were the heavy elements from iron to uranium made?
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How were the heavy elements from iron to uranium made?

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They are released in supernovae, but are made over the life of a star, over many millions and billions of years. The gravitational pressure of a star is so great that it compresses the gasses in its interior to a point that the atoms break down into a plasma state. The atomic nuclei lose their orbiting...
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They are released in supernovae, but are made over the life of a star, over many millions and billions of years. The gravitational pressure of a star is so great that it compresses the gasses in its interior to a point that the atoms break down into a plasma state. The atomic nuclei lose their orbiting electrons into a disassociated soup of particles and groups of particles. The nuclei are forced so close together they sometimes fuse into large nuclei, such as Uranium or other heavy atoms. That is atomic fusion. It releases a tremendous amount of energy and it is what powers stars like our sun. Those nuclei which are inherently unstable break down quickly. Those which are stable may survive in the star until it explodes in a nova or supernova and the heavy elements are released into the nebula. Once the elements are in the nebula, they can condense and coalesce into new planets, stars, and other solar system bodies. Our own solar system is probably a third-generation system, with material from the previous generations stars distributed in the planets, asteroids, and icy objects. We are made of the stuff of dead stars; we are stardust. read less
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The two main contributions are thought to be from the s-process and the r-process, which are both neutron capture processes that are differentiated by their speed relative beta-decay of neutron rich isotopes. Both are end-of-stellar-life processes with the S-process probably happening in the giant...
read more
The two main contributions are thought to be from the s-process and the r-process, which are both neutron capture processes that are differentiated by their speed relative beta-decay of neutron rich isotopes. Both are end-of-stellar-life processes with the S-process probably happening in the giant stages of very heavy stars and the r-process probably happening in core-collapse supernovas. read less
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In supernova explosions.
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They are not made in supernovae. They are released in supernovae, but are made over the life of a star, over many millions and billions of years. The gravitational pressure of a star is so great that it compresses the gasses in its interior to a point that the atoms break down into a plasma state....
read more
They are not made in supernovae. They are released in supernovae, but are made over the life of a star, over many millions and billions of years. The gravitational pressure of a star is so great that it compresses the gasses in its interior to a point that the atoms break down into a plasma state. The atomic nuclei lose their orbiting electrons into a disassociated soup of particles and groups of particles. The nuclei are forced so close together they sometimes fuse into large nuclei, such as Uranium or other heavy atoms. That is atomic fusion. It releases a tremendous amount of energy and it is what powers stars like our sun. Those nuclei which are inherently unstable break down quickly. Those which are stable may survive in the star until it explodes in a nova or supernova and the heavy elements are released into the nebula. Once the elements are in the nebula, they can condense and coalesce into new planets, stars, and other solar system bodies. Our own solar system is probably a third-generation system, with material from the previous generations stars distributed in the planets, asteroids, and icy objects. We are made of the stuff of dead stars; we are stardust. read less
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The two main contributions are thought to be from the s-process and the r-process, which are both neutron capture processes that are differentiated by their speed relative beta-decay of neutron rich isotopes. Both are end-of-stellar-life processes with the S-process probably happening in the giant...
read more
The two main contributions are thought to be from the s-process and the r-process, which are both neutron capture processes that are differentiated by their speed relative beta-decay of neutron rich isotopes. Both are end-of-stellar-life processes with the S-process probably happening in the giant stages of very heavy stars and the r-process probably happening in core-collapse supernovas. read less
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Unlike light elements, which release energy during fusion, elements heavier than iron require energy for their creation. This happens because the nuclear binding energy is at its maximum at iron. Hence lighter elements were made in ordinary stars, using fusion. However, heavier elements were made in...
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Unlike light elements, which release energy during fusion, elements heavier than iron require energy for their creation. This happens because the nuclear binding energy is at its maximum at iron. Hence lighter elements were made in ordinary stars, using fusion. However, heavier elements were made in supernovas, as huge amounts of extra energy are released during the explosion, some of which is used to force heavy nuclei together and create heavier elements. read less
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n novas and supernovas. Collapsing stars are the only objects with enough pressure and energy to fuse heavy atomic nuclei and release them back into space.
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They are not made in supernovae. They are released in supernovae, but are made over the life of a star, over many millions and billions of years. The gravitational pressure of a star is so great that it compresses the gasses in its interior to a point that the atoms break down into a plasma state....
read more
They are not made in supernovae. They are released in supernovae, but are made over the life of a star, over many millions and billions of years. The gravitational pressure of a star is so great that it compresses the gasses in its interior to a point that the atoms break down into a plasma state. The atomic nuclei lose their orbiting electrons into a disassociated soup of particles and groups of particles. The nuclei are forced so close together they sometimes fuse into large nuclei, such as Uranium or other heavy atoms. That is atomic fusion. It releases a tremendous amount of energy and it is what powers stars like our sun. Those nuclei which are inherently unstable break down quickly. Those which are stable may survive in the star until it explodes in a nova or supernova and the heavy elements are released into the nebula. Once the elements are in the nebula, they can condense and coalesce into new planets, stars, and other solar system bodies. Our own solar system is probably a third-generation system, with material from the previous generations stars distributed in the planets, asteroids, and icy objects. We are made of the stuff of dead stars; we are stardust. read less
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They are released in supernovae, but are made over the life of a star, over many millions and billions of years.
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Heavier elements were made in supernovas
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