<p><a href="http://en.wikipedia.org/wiki/Stellar_nucleosynthesis" rel="nofollow">The outer shell of the star</a> contains still a lot of hydrogen, after running out of fuel.</p>

<p>Elements other than hydrogen are denser than hydrogen. This makes it difficult to get hydrogen to the core of a star, or to the region of <a href="http://en.wikipedia.org/wiki/CNO_cycle" rel="nofollow">hydrogen-burning</a> at least, after the core has been burnt to helium or heavier elements.</p>

<p>But the life of a star can be extended in some way, e.g. by adding hydrogen to a white dwarf. This can trigger <a href="http://en.wikipedia.org/wiki/Carbon_burning_process" rel="nofollow">burning of carbon</a> with a <a href="http://en.wikipedia.org/wiki/Type_Ia_supernova" rel="nofollow">supernova Ia</a> as result.</p>

CC BY-SA 3.0
2014-03-02T21:58:12.267Z
2014-03-02T21:58:12.267Z
Gerald
<blockquote>
  <p>If something crashed into it rearranging its content a bit, could its life be extended?</p>
</blockquote>

<p><strong>Yes!</strong> This is precisely what we think causes the creation of <em><a href="https://en.wikipedia.org/wiki/Blue_straggler" rel="noreferrer">blue stragglers</a></em>.</p>

<p>When we look at a cluster of stars, we expect them to all be of roughly the same age.  This is usually borne out by observations.  Because larger stars evolve faster, the age of a cluster can then be roughly determined by working out the mass of the most massive star still on the main sequence (i.e. still burning hydrogen in the core).  We call this the <em>main-sequence turnoff</em>.</p>

<p>But in some clusters, we see and handful of stars that are more massive, but still on the main sequence, even though all the evidence says they should have already evolved into giants and other more-evolved objects.  The consensus view is that these stars are at the very least interacting with binary companions, and many are thought to be <em>merger products</em>. i.e. something left over from two stars merging into one.  Either two companions in a binary have orbited so close that they've become one star, or two stars have simply collided (which is quite possible in the dense cores of clusters).  Depending on what types of star collide, you can basically get a new star where everything is mixed up again, allowing the star to be "born again".</p>

CC BY-SA 3.0
2014-08-24T15:11:11.513Z
+1 this is the only proper answer for this question.
Walter
CC BY-SA 3.0
2014-08-19T09:28:55.173Z
2014-08-19T09:28:55.173Z
Warrick
<p>Stars actually do this on their own, to an extent.  The material inside a star (in some layers) does convect, and at certain points in the star's life, the material in the core can actually rise up and mix with the rest of the star.  This might replenish some H and He in the core, but the main effect that can be observed is that the fusion products become visible at the surface.</p>

<p>Also, the size and location of the convective layers depends very much on stellar size - in a red dwarf the convective zone is most of the star.  That's one reason red dwarf stars live so long - they continually "recycle" their available Hydrogen.</p>

<p><a href="http://en.wikipedia.org/wiki/Star#Structure" rel="nofollow">http://en.wikipedia.org/wiki/Star#Structure</a></p>

<p><a href="http://en.wikipedia.org/wiki/Dredge-up" rel="nofollow">http://en.wikipedia.org/wiki/Dredge-up</a> </p>

CC BY-SA 3.0
2014-08-15T20:14:08.190Z
2014-08-15T20:14:08.190Z
user4815162342
<p>When stars transition from the main sequence core Hydrogen burning to core Helium burning they can experience <a href="http://www.atnf.csiro.au/outreach/education/senior/astrophysics/stellarevolution_postmain.html" rel="nofollow noreferrer">Hydrogen shell burning</a>.  </p>

<p><img src="https://i.sstatic.net/ZxefW.jpg" alt="http://www.atnf.csiro.au/outreach/education/senior/astrophysics/stellarevolution_postmain.html"></p>

<p>However, when you burn the Hydrogen in the shell to Helium, it will fall on the core creating a hotter core where the radiation pressure from the Helium burning core will push the Hydrogen further out into the outer envelope. From here you can get a <a href="http://en.wikipedia.org/wiki/Helium_flash" rel="nofollow noreferrer">Helium flash</a> which is the cause of <a href="http://en.wikipedia.org/wiki/Horizontal_branch" rel="nofollow noreferrer">Horizontal Branch</a> stars.</p>

<p>If you were able to somehow force more Hydrogen to shell burn then you could possibly extend the life for a short while, though the lifetimes post main sequence are much shorter &lt; 1 Gyr compared to the lifetimes on the main sequence.</p>

CC BY-SA 3.0
2015-01-06T03:43:26.513Z
There is no helium burning when a post main sequence star is on the red giant branch. The helium core is initially inert. The helium flash marks when that inert helium core finally ignites.
David Hammen
CC BY-SA 3.0
2014-08-16T00:11:59.510Z
2014-08-16T00:11:59.510Z
Aaron
<p>Is it true that when a star 'runs out' of its fuel, it hasn't really used up all its hydrogen, it still has hydrogen left, but the hydrogen is not at its center where the fusion happens. If something crashed into it rearranging its content a bit, could its life be extended?</p>

CC BY-SA 3.0
2015-08-27T15:48:04.127Z
I suppose in theory you could suck the helium out of the core, but I suspect the technical difficulties would be insurmountable.
Joshua
<star>
Is it possible to extend the life of a star?
bogen
# Is it possible to extend the life of a star?

(Asked by: username_0 on 2014-03-02)

Is it true that when a star 'runs out' of its fuel, it hasn't really used up all its hydrogen, it still has hydrogen left, but the hydrogen is not at its center where the fusion happens. If something crashed into it rearranging its content a bit, could its life be extended?

**Tags:** star
> **Comments:**
> **username_1**: I suppose in theory you could suck the helium out of the core, but I suspect the technical difficulties would be insurmountable.  

---

## 4 answers

### Answer by username_2 on 2014-03-02. Score: 4 | Accepted answer

[The outer shell of the star](http://en.wikipedia.org/wiki/Stellar_nucleosynthesis) contains still a lot of hydrogen, after running out of fuel.

Elements other than hydrogen are denser than hydrogen. This makes it difficult to get hydrogen to the core of a star, or to the region of [hydrogen-burning](http://en.wikipedia.org/wiki/CNO_cycle) at least, after the core has been burnt to helium or heavier elements.

But the life of a star can be extended in some way, e.g. by adding hydrogen to a white dwarf. This can trigger [burning of carbon](http://en.wikipedia.org/wiki/Carbon_burning_process) with a [supernova Ia](http://en.wikipedia.org/wiki/Type_Ia_supernova) as result.


---

### Answer by username_3 on 2014-08-19. Score: 5

> If something crashed into it rearranging its content a bit, could its life be extended?

**Yes!** This is precisely what we think causes the creation of *[blue stragglers](https://en.wikipedia.org/wiki/Blue_straggler)*.

When we look at a cluster of stars, we expect them to all be of roughly the same age. This is usually borne out by observations. Because larger stars evolve faster, the age of a cluster can then be roughly determined by working out the mass of the most massive star still on the main sequence (i.e. still burning hydrogen in the core). We call this the *main-sequence turnoff*.

But in some clusters, we see and handful of stars that are more massive, but still on the main sequence, even though all the evidence says they should have already evolved into giants and other more-evolved objects. The consensus view is that these stars are at the very least interacting with binary companions, and many are thought to be *merger products*. i.e. something left over from two stars merging into one. Either two companions in a binary have orbited so close that they've become one star, or two stars have simply collided (which is quite possible in the dense cores of clusters). Depending on what types of star collide, you can basically get a new star where everything is mixed up again, allowing the star to be "born again".

> **Comments:**
> **username_4**: +1 this is the only proper answer for this question.  

---

### Answer by username_5 on 2014-08-15. Score: 4

Stars actually do this on their own, to an extent. The material inside a star (in some layers) does convect, and at certain points in the star's life, the material in the core can actually rise up and mix with the rest of the star. This might replenish some H and He in the core, but the main effect that can be observed is that the fusion products become visible at the surface.

Also, the size and location of the convective layers depends very much on stellar size - in a red dwarf the convective zone is most of the star. That's one reason red dwarf stars live so long - they continually "recycle" their available Hydrogen.

<http://en.wikipedia.org/wiki/Star#Structure>

<http://en.wikipedia.org/wiki/Dredge-up>


---

### Answer by username_6 on 2014-08-16. Score: 3

When stars transition from the main sequence core Hydrogen burning to core Helium burning they can experience [Hydrogen shell burning](http://www.atnf.csiro.au/outreach/education/senior/astrophysics/stellarevolution_postmain.html).

![http://www.atnf.csiro.au/outreach/education/senior/astrophysics/stellarevolution_postmain.html](https://i.sstatic.net/ZxefW.jpg)

However, when you burn the Hydrogen in the shell to Helium, it will fall on the core creating a hotter core where the radiation pressure from the Helium burning core will push the Hydrogen further out into the outer envelope. From here you can get a [Helium flash](http://en.wikipedia.org/wiki/Helium_flash) which is the cause of [Horizontal Branch](http://en.wikipedia.org/wiki/Horizontal_branch) stars.

If you were able to somehow force more Hydrogen to shell burn then you could possibly extend the life for a short while, though the lifetimes post main sequence are much shorter < 1 Gyr compared to the lifetimes on the main sequence.

> **Comments:**
> **username_7**: There is no helium burning when a post main sequence star is on the red giant branch. The helium core is initially inert. The helium flash marks when that inert helium core finally ignites.  

---

