Why is iron responsible for causing a supernova?

  • Why is the element iron responsible for supernova? Can any star create more element than iron within the span of its life?

    I understand that when star dies due to supernova, other elements are created (Gold and other 92 elements) due to more heat generated than required not only for fusion of Iron element but also for the fusion of higher element with each other.

    You should definitely improve your way to ask questions :) It is very much related to your comprehension of the topic, and to the quality of the answers you will receive. For example: the iron is not "responsible" for supernova, it is the last element produced by nuclear fusion. So you could ask: According to this reference (reference), the iron is the last element produced within star's core, but I don't understand the reason, bla bla bla.

    @Py-ser Iron is not the last element created by fusion. It is the last for which fusion produces energy. Further elements up to Uranium (last natural element) actually consume energy when creating.

    Actually, isn't it Ni which is the last for which fusion produces instead of consumes energy?

    I forgot to mention "in stars", thanks.

    @Jeremy no, it is Fe, but there is quite a plateau from Fe56 to Sr86. What happens with Ni62 is that it is the most tightly bond. http://en.wikipedia.org/wiki/Nuclear_binding_energy#The_binding_energy_maximum_and_ways_to_approach_it_by_decay

    @Jeremy Yes. And what about that?

    So, 56-Ni is the last element created by fusion that produces energy instead of consuming it. This happens to decay to iron... but it is 56-Ni that is the last element produced by fusion producing energy.

  • Your question is a bit oversimplified because there are many types of supernovae based on the size and configuration of the star. But I can answer your question about "why iron" by considering what keeps a star from exploding in the first place.

    In the simplest terms of star formation, when material from an interstellar nebula starts to collapse under its own gravity, the pressure and temperatures involved will become great enough to eventually start fusing hydrogen into helium (it's a bit more complicated than that, but I'm speaking in generalities). If you were to consider the helium atoms created by that process, you'll notice that each helium atom weighs just a bit less than the two hydrogen atoms that formed it. That bit of extra mass is given off as energy which is produced in great quantities as the hydrogen continues to be fused into helium.

    During the star's "main sequence", the release of energy by the hydrogen-helium fusion helps counteract the weight of the star's gasses pushing inward. Material presses in; energy pushes out in perfect balance. This balance of gravity and energy output continues until the star uses up most of its hydrogen.

    It's at this this point (when there is no hydrogen left in the core of the star to fuse into helium) that the fusion reaction stops and gravity will resume to collapse the star further. As this star collapses, it will quickly become denser and hotter until the temperature and pressures of the interior are great enough to start fusing helium into heavier elements… and the process continues.

    That is, until the star starts fusing elements into iron…

    The fusion into iron is the first element that does not create more energy than it takes to produce. The effect is that there is no net energy being produced to counteract the gravity pushing inward. So the outer layers will quickly collapse into a much denser and smaller ball causing the remaining star material to undergo fusion all at once, causing the supernova.

    So, in that sense, iron is not the cause of the supernova, but its presence marks the inevitable end of this star's life cycle… in this particular scenario.

    But understand that this is an oversimplification to illustrate the process you asked about. There are many other sequences of a star's life cycle. Our sun, for example, does not have sufficient mass to keep collapsing down with sufficient pressures to fuse heavier elements into iron. Without getting into other pathways for the production of heavy elements (even in smaller stars like our sun) — once our sun starts creating carbon and oxygen, the fuel starts to run out and the core will simply collapse and rebound as it swells up into a red giant, before losing its outer layers as a planetary nebula while the core shrinks to become a white dwarf (and eventually cooling into a black dwarf).

    @RobertCartaino perhaps you can include some references in your answer? For instance I am interested in a reference supporting the statement *The fusion into iron is the first element that does not create more energy than it takes to produce*

    @Jeremy First a small clarification, iron is the last element that produces a net release of energy by nuclear fusion. Any fusion of/with iron into heavier elements consumes more energy than the process releases. Some sources: NASA Universe 101 on The Life and Death of Stars or Wikipedia on Supernova nucleosynthesis (where you might find other sources in references and suggested reading sections).

    @TidalWave yup, so two things here: it does not require more energy to create Fe by fusion than is released (as stated by Robert), and also that wikipedia link you provide says: *The second, and more common, cause is when a massive star, usually a red giant, reaches nickel-56 in its nuclear fusion (or burning) processes. This isotope undergoes radioactive decay into iron-56* - so it is Nickel, not Iron, that is the last element that produces a net release of energy by fusion (and it happens to decay to Fe).

    As @Robert Cartaino noted, his explanation was condensed for comprehensibility. If you actually trace the chain of nucleosynthesis, (e.g., p22 of http://www.as.utexas.edu/astronomy/education/fall10/scalo/secure/301F10.Ch21Supernovae.SLIDES.pdf) the penultimate species is Fe52 which absorbs one more alpha particle to become Ni56 yielding a tiny amount of energy. Any more alpha absorptions *cost* energy. Ni56 is unstable, decaying to the lower-energy Fe56 with a half-life of about 6 days. When the SN goes bang, there will always be quite a lot of Ni56 that has not yet turned into Fe56.

    When you say 'fusion into iron' does not create more energy it sounds like you mean the fusion of iron. But that does create more energy. Do you mean other elements fusing with iron? That should be cleared up.

    @MarkOlson your comment isn't correct. For example, the addition of an alpha particle to 56Ni, producing 60Zn, is exothermic.

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Content dated before 7/24/2021 11:53 AM