When a star has finished fusing all its hydrogen into helium, it will then start fusing helium into beryllium and so on and so forth up until iron.

When the star is fusing to beryllium, will the star still be in the main sequence phase and will it at that point start to grow into the red giant phase, or is there no given rule for when it will start growing?

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    $\begingroup$ Stars don't fuse helium to beryllium, Be-8 has an extremely short half-life. Beryllium isotopes are produced by cosmic ray spallation. $\endgroup$
    – PM 2Ring
    Commented Nov 5, 2018 at 20:25
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    $\begingroup$ Thx PM for highlighting my mistake, I did some more research and see Small ->H->He, Medium go up to Carbon. However massive stars go up Copper and more, I thought fusion stopped at Iron. enchantedlearning.com/subjects/astronomy/stars/fusion.shtml $\endgroup$ Commented Nov 5, 2018 at 20:33
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    $\begingroup$ You're right: stellar fusion does stop at iron / nickel. But in a hot star with sufficient neutron flux heavier species can be "cooked" by the s-process. $\endgroup$
    – PM 2Ring
    Commented Nov 5, 2018 at 20:54
  • $\begingroup$ @PM2Ring But Be9 is stable. $\endgroup$ Commented Nov 6, 2018 at 19:41
  • $\begingroup$ @Accumulation Sure, but how are you going to build it via fusion? He-4 + He-5 is unlikely, because He-5 has a very short halflife. Be-8 + p -> B-9 just spits the proton back out with an equally tiny halflife. $\endgroup$
    – PM 2Ring
    Commented Nov 6, 2018 at 20:29

2 Answers 2


Does a star fuse helium to beryllium on the main sequence?

Stars don't fuse helium to beryllium except as a very, very short intermediate step toward carbon. Helium-helium fusion to form beryllium is endothermic: It consumes energy. To make matters worse, the beryllium-8 that results has an extremely short half-life, less than $10^{-16}$ seconds. Helium would be the end of fusion in stars (and there would be no us) if not for a fluke: The beryllium-8 formed by helium-helium fusion has almost exactly the same energy as does an excited state of carbon-12.

This greatly increases the probability of a third helium-4 nucleus combining with a short-lived beryllium-8 nucleus to form carbon-12. This is stable. The next stage after hydrogen burning is thus triple helium burning (the triple alpha process), essentially bypassing beryllium except as an intermediary.

When the star is fusing to beryllium, will the star still be in the main sequence phase and will it at that point start to grow into the red giant phase, or is there no given rule for when it will start growing?

A star leaves the main sequence well before it starts fusing helium. It leaves the main sequence when the star can no longer sustain hydrogen fusion in the core. This happens when the core becomes void of hydrogen. At this point, the helium left behind by hydrogen fusion is essentially ash. Hydrogen fusion proceeds on the edge of the core (shell burning), but the hydrogen-depleted core at this point is far too cold to fuse helium to carbon (not beryllium). So it collapses, and gradually becomes hotter.

The star starts fusing helium to carbon (and also oxygen) if the post main sequence star's mass is large enough. At this point, the red giant collapses and behaves almost like a main sequence star with a second life. That second life doesn't last very long, however.


What defines the main sequence?

Main sequence stars are characterized by hydrogen fusion in their cores, either through the proton-proton chain (for lower-mass stars) or the CNO cycle (for stars more than about 1.5 times the Sun's mass). Outside the core, no significant fusion takes place; the outer layers are involved in radiative or convective energy transport, but not energy generation. In general, if hydrogen fusion is occurring in the core, we say that a star is still on the main sequence.

This changes in stars that evolve off the main sequence. Some low-mass red giants may fuse hydrogen to helium via the CNO cycle in a layer outside a largely non-reactive helium core; this is referred to as shell burning. In more massive stars, heavier elements (e.g. helium, carbon, etc.) are fused inside the core, and shell burning continues in the outer layers. For instance, in a fairly high-mass star that is far into the post-main sequence phase of its life, you might see oxygen, neon, carbon, helium and hydrogen being fused in successive layers farther and farther from the core.

A common misconception is that a star uses up all its hydrogen before leaving the main sequence; this is not true. It merely uses up the majority of the hydrogen in its core; there is still plenty in the outer layers, which is what makes shell fusion possible.

Post-main sequence evolution

Let's consider stars of around one solar mass. As hydrogen fusion stops in the (now degenerate) core, the source of pressure keeping the star in hydrostatic equilibrium vanishes. Hydrogen burning starts in a shell around the core. After some time, the core begins to contract, the outer envelope expands, and the star is said to be on the red giant branch. Eventually, temperatures rise to the point where the triple-alpha process can occur, and a helium flash occurs, marking the beginning of the horizontal branch and helium fusion via the triple-alpha process. Hydrogen shell burning continues.

As you'll notice - and as others have said - stars don't fuse helium to beryllium to any significant degree during any part of this process, or post-main sequence evolution in general. It's endothermic; the triple-alpha process is exothermic.

  • $\begingroup$ At what point does a star begin to grow? At the end of hydrogen fusion in the core? $\endgroup$ Commented Nov 5, 2018 at 20:20
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    $\begingroup$ @MiscellaneousUser Stars grow throughout their life in the main sequence. For example, our Sun was only 0.75 R☉ just after its birth, and 3-4 billion years from now it will be around 1.5 R☉. Of course, I assume you are referring to the expansion into a red giant. In that case, it is when helium begins to fuse. Hydrogen still gets fused along the edges of the core, and this is referred to as the Hydrogen-fusion shell, but most of the core will be fusing helium (or heavier elements if later along) at the point. Now, technically, the shell is actually not part of the core, but that's semantics. $\endgroup$
    – User24373
    Commented Nov 5, 2018 at 21:10
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    $\begingroup$ @KITTENDESTROYER-9000 "In that case, it is when helium begins to fuse. " This part of your comment is not right. A star shrinks when it begins to fuse helium and terminates the first ascent red giant branch. $\endgroup$
    – ProfRob
    Commented Nov 5, 2018 at 23:08
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    $\begingroup$ Re the misconception discussed in paragraph 3, pretty much no physical process is going to transform all the A into B, then transform all the B into C and so on. Rather, as A becomes less abundant, the rate of transforming A to B will slow and, as B becomes more abundant, the rate of C production will increase. It's never going to be a hard cut-off. $\endgroup$ Commented Nov 6, 2018 at 18:38

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