<p>To clearify: In your question you distinguish between a star forming a neutron star when its core exceeds the Chandrasekhar limit and a star undergoing a Type II supernova. 
These are, however, the same events. </p>

<p>To summarize: Generally an isolated star can die in one of basically four ways. With increasing probability with increasing mass these outcomes are:</p>

<p><strong>1. Formation of a white dwarf:</strong> This is the outcome for stars with a initial mass below ~10 solar masses and includes our sun. This includes about 97% of all stars, as small stars are the most abundant.<br>
At the end of its lifetime, when it has burned though all the hydrogen accessible to its core, it will start to burn gradually heavier elements in its contracting core. Up to which element this can go depends on the initial mass of the star. During this process the outer layers of the star begin to expands and it enters the red giant phase. At the end of which they shed their outer layers which then form a planetary nebular. All that is left after that is the cooling core of heavier elements. The <a href="http://White%20dwarf" rel="nofollow noreferrer">white dwarf</a>. This white dwarf is held up against gravity by degenerate electron pressure. This means the electrons are so close together that, to contract further, they have to be pushed in an higher energy state to not violate the Pauli exclusion principle. 
An example would be the beautiful Ring Nebular where you can easily see the white dwarf in the middle.  </p>

<p><img src="https://i.sstatic.net/yq2GP.jpg" width="300" height="300"></p>

<p><strong>2. Supernova and the formation of a Neutron star:</strong>
The core of heavier stars (<span class="math-container">$9-100 M_{\odot}$</span>) are, too, mostly held up by degenerate electron. During the lifetime of the star more and more heavy elements collect in a growing core. With increasing core mass/density, however, the electrons reach higher and higher energies. At some point these energies become high enough for electrons to be "pushed" into protons, becoming neutrons and releasing lots neutrinos in the process. This reduces the degenerate pressure until it can no longer support the core against the gravitational pressure of the outer layers.
This happens when the core exceeds the mentioned <a href="https://en.wikipedia.org/wiki/Chandrasekhar_limit" rel="nofollow noreferrer">Chandrasekhar limit</a>. This is what initializes the core-collapse of heavier stars.  </p>

<p>Even heavier stars with hotter cores are increasing held up not only by degenerate pressure but regular thermal pressure. For those stars the collapse is additionally promoted when photodisintegration of heavy elements saps the core of more and more thermal energy and leads to its further contraction.
(See the first pages <a href="https://arxiv.org/pdf/1206.2503.pdf" rel="nofollow noreferrer">here</a> for a more detailed description of how the SN is triggered)  </p>

<p>Independent from how the collapse started, it continues until at some point the degenerate neutron pressure and most importantly the <a href="https://www.forbes.com/sites/startswithabang/2018/06/13/the-surprising-reason-why-neutron-stars-dont-all-collapse-to-form-black-holes/#947523f7159c" rel="nofollow noreferrer">repulsion of the strong nuclear force</a> kicks in. 
At this point the core-collapse suddenly halts and the proto-neutron star becomes virtually incompressible. This all happens so fast, that the outer shells basically free-fall onto the proto-NS and "bounce off". Together with the energy provided by the intense neutrino flux, this drives away the outer shells and leads to the explosion of the star. This is a <a href="https://www.mpa-garching.mpg.de/84411/Core-collapse-supernovae" rel="nofollow noreferrer">core-collapse supernova</a>. All that is left is a expanding supernova remnant and a central neutron star, a pulsar. The composition of the remaining outer layers at the time of the explosion determines the type of the SN.<br>
Most famous example: The Crab nebular.   </p>

<p><img src="https://i.sstatic.net/CH0uN.jpg" width="300" height="300"></p>

<p><strong>3. Core-collapse SN with black hole formation:</strong>
At higher masses it can happen that not all of the outer layers can escape the gravitational well of the proto-NS. Some part of it can fall back onto it. During this process the NS can gain mass again and eventually exceed the <a href="https://en.wikipedia.org/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" rel="nofollow noreferrer">Oppenheimer-Volkoff-Limit</a>. When this happens even the pressure from the degenerate neutron gas is not sufficient anymore. At this point there is nothing that can stop the gravitational collapse to a black hole. The accretion of the additional material again releases huge amounts of energy and can lead to the formation of jets. This is what is suspected to be a <a href="http://astronomy.swin.edu.au/cosmos/H/Hypernova" rel="nofollow noreferrer">Hypernova</a> and can be accompanied by a gamma ray burst (GRB).<br>
See below for and animation of a jet braking though the expanding supernova shell and producing a GRB:</p>

<p><a href="https://i.sstatic.net/biLuD.gif" rel="nofollow noreferrer"><img src="https://i.sstatic.net/biLuD.gif" alt="enter image description here"></a></p>

<p><strong>4. Core-collapse with direct BH formation:</strong>
An alternative, less violent way for forming a BH is a direct collapse. This mostly happens for very heavy stars. 
In this scenario the proto-neutron star is unable to initialize the ejection of the outer layers and just collapses to a BH. No huge explosion, no supernova remnant. 
This is sometimes called a <a href="https://en.wikipedia.org/wiki/Failed_supernova" rel="nofollow noreferrer">failed supernova</a>. And we have actually seen such a <a href="https://en.wikipedia.org/wiki/N6946-BH1" rel="nofollow noreferrer">star</a> just disappearing:</p>

<p><a href="https://i.sstatic.net/F5nDc.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/F5nDc.jpg" alt="failed supernova"></a></p>

<p><strong>5. Pair-instability supernova and complete disruption:</strong>
For stars with masses between about <a href="https://arxiv.org/abs/astro-ph/0212469" rel="nofollow noreferrer">140 and 260 <span class="math-container">$M_{\odot}$</span></a> (see respective gap in the figure below) temperatures in the core can become hot enough that thermal radiation reaches gamma ray energies. Specifically photons can reach energies high enough to produce e<span class="math-container">$^-$</span>/e<span class="math-container">$^+$</span> pairs. This process transfers thermal energy into the mass of the formed particles. This leads to a contraction of the core. At that stage the core has not jet fused many heavy elements and consists mostly of Helium, which now undergoes rapid fusion as the core contracts. The released energy complete disrupts the stars leaving no compact core and only an expanding shell. Such heavy stars mostly formed in the early universe as the first generation of stars. </p>

<hr>

<p>Which one of the scenarios 2 - 4 will happen to a star with a zero-age main-sequence (ZAMS) mass of more than 15 solar masses is hard to tell and an active field of research. It all depends on ZAMS mass, binarity, metallicity, angular momentum, and magnetic fields, among others properties of the progenitor star. Current computational capabilities are just not enough to produce reliable 3D magneto-hydrodynamic simulations with good temporal and spacial resolution and scale. </p>

<p>But from <a href="https://arxiv.org/abs/astro-ph/0212469" rel="nofollow noreferrer">here</a> there is a rough estimate of what we think is the most probable outcome for different masses and metallicities:  </p>

<p><img src="https://i.sstatic.net/ezRp2.jpg" width="700" height="450"></p>

<p>And from <a href="https://arxiv.org/abs/1510.04643" rel="nofollow noreferrer">here</a> there is a set of actual 1D simulations of the supernova 1987A showing all kinds of different outcomes for different masses and initial models of the star:<br>
(Although 1D simulations tend to have a hard time to initialize explosions)
<img src="https://i.sstatic.net/lmvLc.png" width="500" height="300"></p>

<p>How complex these simulations are can also be seen in nice 3D videos like <a href="https://www.youtube.com/watch?v=6r7YUj42SJ0" rel="nofollow noreferrer">this one</a>. </p>

<p>So you see, to determine which stars go through which final fate we have to torture huge supercomputers and even then we still have a hard time coming up with definitive answers. </p>

CC BY-SA 4.0
2019-09-04T19:55:25.850Z
This is not a bad summary, but a point of correction. Neutron stars, as was shown by work in the 1930s, cannot be supported by neutron degeneracy pressure if they exceed 0.7 solar masses. The core bounce and ultimate support of any neutron star remnant is predominantly due to the strong force repulsion between tightly packed neutrons.
ProfRob
CC BY-SA 4.0
2019-09-04T20:52:00.197Z
Thanks, good point. I will change that. But I am surprised how often only degenerate pressure is mentioned.
SpaceCore
CC BY-SA 4.0
2019-09-04T21:19:20.423Z
Mentioned where? Not in any reputable textbook or journal paper. See Oppenheimer & Volkhoff **1939**. https://journals.aps.org/pr/abstract/10.1103/PhysRev.55.374
ProfRob
CC BY-SA 4.0
2019-09-04T21:29:21.673Z
Not paper and textbooks, but popular science articles, Q&A posts and even my old (but not that old) lecture slides.
SpaceCore
CC BY-SA 4.0
2019-09-05T06:44:36.367Z
+1 For completeness you could add the pair production instability supernova outcome at very high masses, which may determine the upper limit to the mass of black holes produced by massive stars.
ProfRob
CC BY-SA 4.0
2019-09-05T13:11:22.800Z
Thanks, I added a few lines about that.
SpaceCore
CC BY-SA 4.0
2019-09-06T17:08:43.817Z
This contains two remarkable facts I didn't realize-- that we have actually seen a star disappear that can be interpreted as implosion into a black hole, and that it seems as stars are getting higher and higher metallicity with time, equaling or exceeding solar metallicity, it may be that the universe no longer creates black holes in supernovae.
Ken G
CC BY-SA 4.0
2019-09-06T17:10:32.133Z
A minor point to bear in mind because it creates many misconceptions.  It is easy to imagine that degeneracy pressure means that because electrons cannot be in the same state, this creates some bizarre "repulsion" between them.  That isn't true, the inability to occupy the same state means that electrons cannot lose any more heat, which prevents further contraction.   The pressure is there for all the usual reasons-- the electrons get a lot of kinetic energy during the contraction that does happen.
Ken G
CC BY-SA 4.0
2019-09-04T15:57:11.287Z
2019-09-05T13:10:08.697Z
2019-09-05T13:10:08.697Z
SpaceCore
<p>I am reading about massive stars and their final consequences. what I understood is massive stars after throwing out their outer envelop with masses > 1.4 solar Mass turn into neutron stars. But I also know that Massive stars can collapse to form a type II supernova. I need to understand how we determine which stars go through which final fate. And what initial mass they have to start their life with for both fates.</p>

<p>I ma be completely wrong with my understandings. Your clarifications will help a lot. </p>

CC BY-SA 3.0
2018-02-15T18:35:42.527Z
The Chandrasekhar limit of 1.4 solar masses is the maximum mass of a white dwarf; if the remnant has a mass greater than that, it will collapse instead into a neutron star or black hole. However, this maximum isn't directly related to the mass of the progenitor star; stars with, say, 2 solar masses can still form white dwarfs.
HDE 226868
CC BY-SA 3.0
2018-02-15T18:47:50.200Z
A related question here, Rob Jeffries gave me a very nice answer.   https://astronomy.stackexchange.com/questions/12205/how-massive-does-a-main-sequence-star-need-to-be-to-go-type-1-supernova.
userLTK
CC BY-SA 3.0
2018-02-15T18:53:09.150Z
If interested, here's a nice short summary that may miss on some of the latest research, but it covers the basics:   https://phys.org/news/2016-03-kinds-supernovae.html
userLTK
CC BY-SA 3.0
2018-02-28T09:46:50.947Z
The only way to get a neutron star is for the core of a massive star to collapse -- which triggers a supernova. So it's the *same* fate. (The supernova will be Type II if there's still a hydrogen envelope outside the core; if the outer, hydrogen-containing envelope was previously ejected, then it will be a Type Ib or Ic supernova.)
Peter Erwin
<star><supernova><neutron-star>
Core collapse supernova vs Neutron Star
bhjghjh
# Core collapse supernova vs Neutron Star

(Asked by: username_0 on 2018-02-15)

I am reading about massive stars and their final consequences. what I understood is massive stars after throwing out their outer envelop with masses > 1.4 solar Mass turn into neutron stars. But I also know that Massive stars can collapse to form a type II supernova. I need to understand how we determine which stars go through which final fate. And what initial mass they have to start their life with for both fates.

I ma be completely wrong with my understandings. Your clarifications will help a lot.

**Tags:** star, supernova, neutron-star
> **Comments:**
> **username_1**: The Chandrasekhar limit of 1.4 solar masses is the maximum mass of a white dwarf; if the remnant has a mass greater than that, it will collapse instead into a neutron star or black hole. However, this maximum isn't directly related to the mass of the progenitor star; stars with, say, 2 solar masses can still form white dwarfs.  
> **username_2**: A related question here, Rob Jeffries gave me a very nice answer.   https://astronomy.stackexchange.com/questions/12205/how-massive-does-a-main-sequence-star-need-to-be-to-go-type-1-supernova.  
> **username_2**: If interested, here's a nice short summary that may miss on some of the latest research, but it covers the basics:   https://phys.org/news/2016-03-kinds-supernovae.html  
> **username_3**: The only way to get a neutron star is for the core of a massive star to collapse -- which triggers a supernova. So it's the *same* fate. (The supernova will be Type II if there's still a hydrogen envelope outside the core; if the outer, hydrogen-containing envelope was previously ejected, then it will be a Type Ib or Ic supernova.)  

---

## 1 answers

### Answer by username_4 on 2019-09-04. Score: 7

To clearify: In your question you distinguish between a star forming a neutron star when its core exceeds the Chandrasekhar limit and a star undergoing a Type II supernova.
These are, however, the same events.

To summarize: Generally an isolated star can die in one of basically four ways. With increasing probability with increasing mass these outcomes are:

**1. Formation of a white dwarf:** This is the outcome for stars with a initial mass below ~10 solar masses and includes our sun. This includes about 97% of all stars, as small stars are the most abundant.  
At the end of its lifetime, when it has burned though all the hydrogen accessible to its core, it will start to burn gradually heavier elements in its contracting core. Up to which element this can go depends on the initial mass of the star. During this process the outer layers of the star begin to expands and it enters the red giant phase. At the end of which they shed their outer layers which then form a planetary nebular. All that is left after that is the cooling core of heavier elements. The [white dwarf](http://White%20dwarf). This white dwarf is held up against gravity by degenerate electron pressure. This means the electrons are so close together that, to contract further, they have to be pushed in an higher energy state to not violate the Pauli exclusion principle.
An example would be the beautiful Ring Nebular where you can easily see the white dwarf in the middle.

![](https://i.sstatic.net/yq2GP.jpg)

**2. Supernova and the formation of a Neutron star:**
The core of heavier stars ($9-100 M\_{\odot}$) are, too, mostly held up by degenerate electron. During the lifetime of the star more and more heavy elements collect in a growing core. With increasing core mass/density, however, the electrons reach higher and higher energies. At some point these energies become high enough for electrons to be "pushed" into protons, becoming neutrons and releasing lots neutrinos in the process. This reduces the degenerate pressure until it can no longer support the core against the gravitational pressure of the outer layers.
This happens when the core exceeds the mentioned [Chandrasekhar limit](https://en.wikipedia.org/wiki/Chandrasekhar_limit). This is what initializes the core-collapse of heavier stars.

Even heavier stars with hotter cores are increasing held up not only by degenerate pressure but regular thermal pressure. For those stars the collapse is additionally promoted when photodisintegration of heavy elements saps the core of more and more thermal energy and leads to its further contraction.
(See the first pages [here](https://arxiv.org/pdf/1206.2503.pdf) for a more detailed description of how the SN is triggered)

Independent from how the collapse started, it continues until at some point the degenerate neutron pressure and most importantly the [repulsion of the strong nuclear force](https://www.forbes.com/sites/startswithabang/2018/06/13/the-surprising-reason-why-neutron-stars-dont-all-collapse-to-form-black-holes/#947523f7159c) kicks in.
At this point the core-collapse suddenly halts and the proto-neutron star becomes virtually incompressible. This all happens so fast, that the outer shells basically free-fall onto the proto-NS and "bounce off". Together with the energy provided by the intense neutrino flux, this drives away the outer shells and leads to the explosion of the star. This is a [core-collapse supernova](https://www.mpa-garching.mpg.de/84411/Core-collapse-supernovae). All that is left is a expanding supernova remnant and a central neutron star, a pulsar. The composition of the remaining outer layers at the time of the explosion determines the type of the SN.  
Most famous example: The Crab nebular.

![](https://i.sstatic.net/CH0uN.jpg)

**3. Core-collapse SN with black hole formation:**
At higher masses it can happen that not all of the outer layers can escape the gravitational well of the proto-NS. Some part of it can fall back onto it. During this process the NS can gain mass again and eventually exceed the [Oppenheimer-Volkoff-Limit](https://en.wikipedia.org/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit). When this happens even the pressure from the degenerate neutron gas is not sufficient anymore. At this point there is nothing that can stop the gravitational collapse to a black hole. The accretion of the additional material again releases huge amounts of energy and can lead to the formation of jets. This is what is suspected to be a [Hypernova](http://astronomy.swin.edu.au/cosmos/H/Hypernova) and can be accompanied by a gamma ray burst (GRB).  
See below for and animation of a jet braking though the expanding supernova shell and producing a GRB:

[![enter image description here](https://i.sstatic.net/biLuD.gif)](https://i.sstatic.net/biLuD.gif)

**4. Core-collapse with direct BH formation:**
An alternative, less violent way for forming a BH is a direct collapse. This mostly happens for very heavy stars.
In this scenario the proto-neutron star is unable to initialize the ejection of the outer layers and just collapses to a BH. No huge explosion, no supernova remnant.
This is sometimes called a [failed supernova](https://en.wikipedia.org/wiki/Failed_supernova). And we have actually seen such a [star](https://en.wikipedia.org/wiki/N6946-BH1) just disappearing:

[![failed supernova](https://i.sstatic.net/F5nDc.jpg)](https://i.sstatic.net/F5nDc.jpg)

**5. Pair-instability supernova and complete disruption:**
For stars with masses between about [140 and 260 $M\_{\odot}$](https://arxiv.org/abs/astro-ph/0212469) (see respective gap in the figure below) temperatures in the core can become hot enough that thermal radiation reaches gamma ray energies. Specifically photons can reach energies high enough to produce e$^-$/e$^+$ pairs. This process transfers thermal energy into the mass of the formed particles. This leads to a contraction of the core. At that stage the core has not jet fused many heavy elements and consists mostly of Helium, which now undergoes rapid fusion as the core contracts. The released energy complete disrupts the stars leaving no compact core and only an expanding shell. Such heavy stars mostly formed in the early universe as the first generation of stars.

---

Which one of the scenarios 2 - 4 will happen to a star with a zero-age main-sequence (ZAMS) mass of more than 15 solar masses is hard to tell and an active field of research. It all depends on ZAMS mass, binarity, metallicity, angular momentum, and magnetic fields, among others properties of the progenitor star. Current computational capabilities are just not enough to produce reliable 3D magneto-hydrodynamic simulations with good temporal and spacial resolution and scale.

But from [here](https://arxiv.org/abs/astro-ph/0212469) there is a rough estimate of what we think is the most probable outcome for different masses and metallicities:

![](https://i.sstatic.net/ezRp2.jpg)

And from [here](https://arxiv.org/abs/1510.04643) there is a set of actual 1D simulations of the supernova 1987A showing all kinds of different outcomes for different masses and initial models of the star:  
(Although 1D simulations tend to have a hard time to initialize explosions)
![](https://i.sstatic.net/lmvLc.png)

How complex these simulations are can also be seen in nice 3D videos like [this one](https://www.youtube.com/watch?v=6r7YUj42SJ0).

So you see, to determine which stars go through which final fate we have to torture huge supercomputers and even then we still have a hard time coming up with definitive answers.

> **Comments:**
> **username_5**: This is not a bad summary, but a point of correction. Neutron stars, as was shown by work in the 1930s, cannot be supported by neutron degeneracy pressure if they exceed 0.7 solar masses. The core bounce and ultimate support of any neutron star remnant is predominantly due to the strong force repulsion between tightly packed neutrons.  
> **username_4**: Thanks, good point. I will change that. But I am surprised how often only degenerate pressure is mentioned.  
> **username_5**: Mentioned where? Not in any reputable textbook or journal paper. See Oppenheimer & Volkhoff **1939**. https://journals.aps.org/pr/abstract/10.1103/PhysRev.55.374  
> **username_4**: Not paper and textbooks, but popular science articles, Q&A posts and even my old (but not that old) lecture slides.  
> **username_5**: +1 For completeness you could add the pair production instability supernova outcome at very high masses, which may determine the upper limit to the mass of black holes produced by massive stars.  
> **username_4**: Thanks, I added a few lines about that.  
> **username_6**: This contains two remarkable facts I didn't realize-- that we have actually seen a star disappear that can be interpreted as implosion into a black hole, and that it seems as stars are getting higher and higher metallicity with time, equaling or exceeding solar metallicity, it may be that the universe no longer creates black holes in supernovae.  
> **username_6**: A minor point to bear in mind because it creates many misconceptions.  It is easy to imagine that degeneracy pressure means that because electrons cannot be in the same state, this creates some bizarre "repulsion" between them.  That isn't true, the inability to occupy the same state means that electrons cannot lose any more heat, which prevents further contraction.   The pressure is there for all the usual reasons-- the electrons get a lot of kinetic energy during the contraction that does happen.  

---

