<p>A white dwarf is a stellar remanent which consists of primarily carbon and oxygen or helium, and is too small in order to fuse those to heavier elements and has too little hydrogen left so that there is no hydrogen shell burning anymore either.</p>
<p>It will end in a <a href="https://en.wikipedia.org/wiki/Type_Ia_supernova" rel="nofollow noreferrer">supernova type Ia</a> when it <em>exceeds</em> the mass limit for a white dwarf of about 1.4 solar masses (the so-called <a href="https://en.wikipedia.org/wiki/Chandrasekhar_limit" rel="nofollow noreferrer">Chandrasekhar limit</a>) - the limit when it actually becomes heavy enough to start fusing the helium and/or carbon in its core. When it starts to exceed this limit due to accretion the fusion reaction will onset so heavily that nothing will remain of the white dwarf and we will see a supernova.</p>
<p>However, if a white dwarf <em>below</em> this mass limit accretes further hydrogen, e.g. from its companion in a multiple system, it will occasionally and usually periodically amass enough hydrogen in its atmosphere so that the hydrogen content is enough that it temporarily starts hydrogen shell burning; this event is then visible as a <a href="https://en.wikipedia.org/wiki/Nova" rel="nofollow noreferrer">nova</a>.</p>
<p>The exact physics are not trivial, and also not every detail is fully understood so far of every of these processes - especially as different systems and mechanisms might interact so that several effects can overlap.</p>

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2024-03-20T12:01:54.683Z
2024-03-20T12:08:06.260Z
2024-03-20T12:08:06.260Z
planetmaker
<p>Obviously, when a white dwarf goes truly supernova, there is nothing left, not even, I have heard, a neutron star or black hole...</p>
<p>But when certain white dwarf stars accrete certain amounts or types of matter, they explode fairly violently, but not as violently as a type 1a supernova, and the white dwarf is still there...</p>
<p>Why is this so?</p>
<p>Is the accreting material different in a regular nova?  Thereby causing it to explode prematurely?  So it can live to explode again another day?</p>
<p>Other than differences in the accreting material (or maybe the exact composition of the dwarf itself), I cannot imagine what the difference is...</p>

<astrophysics><supernova><stellar-astrophysics><white-dwarf><nova>
Why does a white dwarf sometimes go 'nova' and sometimes supernova (type 1a)?
Kurt Hikes
# Why does a white dwarf sometimes go 'nova' and sometimes supernova (type 1a)?

(Asked by: username_0 on 2024-03-20)

Obviously, when a white dwarf goes truly supernova, there is nothing left, not even, I have heard, a neutron star or black hole...

But when certain white dwarf stars accrete certain amounts or types of matter, they explode fairly violently, but not as violently as a type 1a supernova, and the white dwarf is still there...

Why is this so?

Is the accreting material different in a regular nova? Thereby causing it to explode prematurely? So it can live to explode again another day?

Other than differences in the accreting material (or maybe the exact composition of the dwarf itself), I cannot imagine what the difference is...

**Tags:** astrophysics, supernova, stellar-astrophysics, white-dwarf, nova


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## 1 answers

### Answer by username_1 on 2024-03-20. Score: 4

A white dwarf is a stellar remanent which consists of primarily carbon and oxygen or helium, and is too small in order to fuse those to heavier elements and has too little hydrogen left so that there is no hydrogen shell burning anymore either.

It will end in a [supernova type Ia](https://en.wikipedia.org/wiki/Type_Ia_supernova) when it *exceeds* the mass limit for a white dwarf of about 1.4 solar masses (the so-called [Chandrasekhar limit](https://en.wikipedia.org/wiki/Chandrasekhar_limit)) - the limit when it actually becomes heavy enough to start fusing the helium and/or carbon in its core. When it starts to exceed this limit due to accretion the fusion reaction will onset so heavily that nothing will remain of the white dwarf and we will see a supernova.

However, if a white dwarf *below* this mass limit accretes further hydrogen, e.g. from its companion in a multiple system, it will occasionally and usually periodically amass enough hydrogen in its atmosphere so that the hydrogen content is enough that it temporarily starts hydrogen shell burning; this event is then visible as a [nova](https://en.wikipedia.org/wiki/Nova).

The exact physics are not trivial, and also not every detail is fully understood so far of every of these processes - especially as different systems and mechanisms might interact so that several effects can overlap.


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