<p>If you slam a white dwarf into a main-sequence star or red giant such that the white dwarf becomes the core you'd get... a red giant (or supergiant).</p>

<p>Perhaps that sounds odd but basically the cores of low-mass red giants are electron degenerate.  They roughly consist of deep convective envelopes sitting on top of (helium) white dwarfs separated by a thin but intense shell of material undergoing nuclear reactions.  Of course, most real white dwarfs are of the carbon-oxygen variety, so I imagine what you'd really get is something more like an asymptotic giant branch (AGB) star.  But these are also basically red giants too.  Off-hand, I can't say whether the second burning shell (hydrogen into helium) will be present.</p>

<p>Anyway, composition wise things might be a bit different to ordinary red giants, red supergiants or AGB stars but the overall structure will be similar: a dense, degenerate core shrouded in a big sparse envelope.</p>

<p>As for the Chandrasekhar limit, that only defines what happens to a degenerate object.  If the white dwarf is massive enough, then once in equilibrium it would presumably start burning carbon and oxygen into heavier metals, just like a red supergiant.</p>

<p>As a final note, a quick search didn't turn up any literature on this. I know of material about mergers between two white dwarfs or two non-degenerate stars but I couldn't find anything on WD+MS (or similar) mergers.</p>

CC BY-SA 3.0
2016-04-07T06:40:01.837Z
2016-04-07T06:40:01.837Z
Warrick
<p>The outer layers of the star will fall onto the white dwarf, forming an accretion disk as the star stuff spirals in. Like this image shows.</p>

<p><a href="https://i.sstatic.net/ulE45.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/ulE45.jpg" alt="Main sequence star dumping matter onto a white dwarf"></a></p>

<p>When the white dwarf steals enough material to get bigger than 1.4 solar masses, the dwarf will become a <a href="https://en.wikipedia.org/wiki/Supernova#Normal_Type_Ia" rel="nofollow noreferrer">Type Ia supernova</a>. This is probably why we never (rarely?) see Thorne–Żytkow objects made from a white dwarf instead.</p>

<p>If the white dwarf actually collides with its companion star before it explodes as a supernova, I could imagine it would fall into the center as the stellar material drags down the orbit of the white dwarf. Maybe then it will form something like a Thorne–Żytkow object. Or maybe it will accumulate enough material as it falls in to create a neutron star, at which point it blows itself apart in Type II supernova.</p>

CC BY-SA 3.0
2016-04-07T06:36:43.927Z
2016-04-07T06:36:43.927Z
RichS
<p>Thorne and Żytkow's <a href="http://adsabs.harvard.edu/abs/1977ApJ...212..832T" rel="nofollow noreferrer">original paper</a> on TŻOs actually opens with a comparison of TŻOs and the type of object you mention, with a  white dwarf degenerate core instead of a neutron star degenerate core. They note that the equilibrium states - essentially, stable configurations - of such combinations lie near the <a href="https://en.wikipedia.org/wiki/Hayashi_track" rel="nofollow noreferrer">Hayashi track</a> (actually acting a bit like AGB stars, in some cases), indicating high metallicity, as is the case with TŻOs.</p>
<p>These objects generate energy the same way TŻOs do: matter is accreted by the core, releasing gravitational potential energy, and the red giant envelope continues some fusion, although, of course, core fusion has been substantially disrupted by the arrival of the new degenerate core. The main difference in energy production are the ratios between nuclear contributions to luminosity and gravitational contributions to luminosity:
<span class="math-container">$$L_{\text{nuc}}/L\approx0.99,\quad L_{\text{grav}}/L\approx0.01\quad\text{for white dwarf core}$$</span>
<span class="math-container">$$L_{\text{nuc}}/L\approx0.04,\quad L_{\text{grav}}/L\approx0.96\quad\text{for neutron core}$$</span>
Why the difference? <span class="math-container">$L_{\text{grav}}$</span> is proportional to
<span class="math-container">$$\frac{GM_c}{R_cc^2}$$</span>
where <span class="math-container">$_c$</span> refers to values for the core. The masses and radii of neutron stars differ drastically from those of white dwarfs. This becomes less important in the case of supergiant TŻOs (i.e. <span class="math-container">$M&gt;10 M_{\odot}$</span>), because convection cycles &quot;burned&quot; nuclear fuel back outwards into the envelope, and so energy ratios become more like those found in the case of a white dwarf core.</p>
<p>This difference in energy production ratios also means that the objects will remain in roughly stable states for different amounts of time; red giants with white dwarf cores can survive in equilibrium for at least an order of magnitude or more as long as TŻOs.</p>
<p>One interesting thing to note is that TŻOs and red giants with white dwarf cores may share some of the same problems when it comes to stability. The envelopes are expected to be composed similarly and act similarly, with the potential difference in nuclear fusion rates, and so the same dynamical instabilities are possible in both cases. However, Thorne and Żytkow state that they find this possibility unlikely.</p>

CC BY-SA 4.0
2016-04-07T22:16:15.870Z
2020-11-29T00:28:30.023Z
2020-11-29T00:28:30.023Z
HDE 226868
<p><a href="https://en.wikipedia.org/wiki/Thorne%E2%80%93%C5%BBytkow_object">Thorne–Żytkow objects</a> (TZOs) form from collisions between neutron stars and main sequence or giant stars. Ultimately, the neutron star becomes the "core" of the giant star.</p>

<p>However, could this also happen with white dwarfs, if the combined mass is below the TOV limit? White dwarfs are degenerate stars, just like neutron stars, so would they be able to replace the star core in the same way? Would anything happen to the white dwarf if the combined mass is beyond the Chandrasekhar limit?</p>

<star><neutron-star><white-dwarf><stellar-dynamics><thorne-zytkow-object>
If a white dwarf collides with a giant star, could it create a TZO?
Sir Cumference
# If a white dwarf collides with a giant star, could it create a TZO?

(Asked by: username_0 on 2016-04-07)

[Thorne–Żytkow objects](https://en.wikipedia.org/wiki/Thorne%E2%80%93%C5%BBytkow_object) (TZOs) form from collisions between neutron stars and main sequence or giant stars. Ultimately, the neutron star becomes the "core" of the giant star.

However, could this also happen with white dwarfs, if the combined mass is below the TOV limit? White dwarfs are degenerate stars, just like neutron stars, so would they be able to replace the star core in the same way? Would anything happen to the white dwarf if the combined mass is beyond the Chandrasekhar limit?

**Tags:** star, neutron-star, white-dwarf, stellar-dynamics, thorne-zytkow-object

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## 3 answers

### Answer by username_3 on 2016-04-07. Score: 5 | Accepted answer

Thorne and Żytkow's [original paper](http://adsabs.harvard.edu/abs/1977ApJ...212..832T) on TŻOs actually opens with a comparison of TŻOs and the type of object you mention, with a white dwarf degenerate core instead of a neutron star degenerate core. They note that the equilibrium states - essentially, stable configurations - of such combinations lie near the [Hayashi track](https://en.wikipedia.org/wiki/Hayashi_track) (actually acting a bit like AGB stars, in some cases), indicating high metallicity, as is the case with TŻOs.

These objects generate energy the same way TŻOs do: matter is accreted by the core, releasing gravitational potential energy, and the red giant envelope continues some fusion, although, of course, core fusion has been substantially disrupted by the arrival of the new degenerate core. The main difference in energy production are the ratios between nuclear contributions to luminosity and gravitational contributions to luminosity:
$$L\_{\text{nuc}}/L\approx0.99,\quad L\_{\text{grav}}/L\approx0.01\quad\text{for white dwarf core}$$
$$L\_{\text{nuc}}/L\approx0.04,\quad L\_{\text{grav}}/L\approx0.96\quad\text{for neutron core}$$
Why the difference? $L\_{\text{grav}}$ is proportional to
$$\frac{GM\_c}{R\_cc^2}$$
where $\_c$ refers to values for the core. The masses and radii of neutron stars differ drastically from those of white dwarfs. This becomes less important in the case of supergiant TŻOs (i.e. $M>10 M\_{\odot}$), because convection cycles "burned" nuclear fuel back outwards into the envelope, and so energy ratios become more like those found in the case of a white dwarf core.

This difference in energy production ratios also means that the objects will remain in roughly stable states for different amounts of time; red giants with white dwarf cores can survive in equilibrium for at least an order of magnitude or more as long as TŻOs.

One interesting thing to note is that TŻOs and red giants with white dwarf cores may share some of the same problems when it comes to stability. The envelopes are expected to be composed similarly and act similarly, with the potential difference in nuclear fusion rates, and so the same dynamical instabilities are possible in both cases. However, Thorne and Żytkow state that they find this possibility unlikely.


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### Answer by username_1 on 2016-04-07. Score: 3

If you slam a white dwarf into a main-sequence star or red giant such that the white dwarf becomes the core you'd get... a red giant (or supergiant).

Perhaps that sounds odd but basically the cores of low-mass red giants are electron degenerate. They roughly consist of deep convective envelopes sitting on top of (helium) white dwarfs separated by a thin but intense shell of material undergoing nuclear reactions. Of course, most real white dwarfs are of the carbon-oxygen variety, so I imagine what you'd really get is something more like an asymptotic giant branch (AGB) star. But these are also basically red giants too. Off-hand, I can't say whether the second burning shell (hydrogen into helium) will be present.

Anyway, composition wise things might be a bit different to ordinary red giants, red supergiants or AGB stars but the overall structure will be similar: a dense, degenerate core shrouded in a big sparse envelope.

As for the Chandrasekhar limit, that only defines what happens to a degenerate object. If the white dwarf is massive enough, then once in equilibrium it would presumably start burning carbon and oxygen into heavier metals, just like a red supergiant.

As a final note, a quick search didn't turn up any literature on this. I know of material about mergers between two white dwarfs or two non-degenerate stars but I couldn't find anything on WD+MS (or similar) mergers.


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### Answer by username_2 on 2016-04-07. Score: 1

The outer layers of the star will fall onto the white dwarf, forming an accretion disk as the star stuff spirals in. Like this image shows.

[![Main sequence star dumping matter onto a white dwarf](https://i.sstatic.net/ulE45.jpg)](https://i.sstatic.net/ulE45.jpg)

When the white dwarf steals enough material to get bigger than 1.4 solar masses, the dwarf will become a [Type Ia supernova](https://en.wikipedia.org/wiki/Supernova#Normal_Type_Ia). This is probably why we never (rarely?) see Thorne–Żytkow objects made from a white dwarf instead.

If the white dwarf actually collides with its companion star before it explodes as a supernova, I could imagine it would fall into the center as the stellar material drags down the orbit of the white dwarf. Maybe then it will form something like a Thorne–Żytkow object. Or maybe it will accumulate enough material as it falls in to create a neutron star, at which point it blows itself apart in Type II supernova.


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