<p>Hydrodynamic models of the Sun allow one method of estimating its internal properties. To do this, the Mass, radius, surface temperature, and total luminosity (radiative energy emitted)/s of the Sun must be known (determined observationally). Making several assumptions, e.g., that the Sun behaves as a fluid and that local thermodynamic equilibrium applies, the stellar equations of state can be used. Numerical methods are applied to these equations to determine the internal properties of the Sun, such as its central temperature. </p>

<p>A great example for how to work this problem your self can be found in the undergraduate text, 'An Introduction to Modern Astrophysics' by Carroll and Ostlie (Section 10.5). The FORTRAN code to run your own stellar model is included in Appendix H. </p>

<p>A comprehensive review paper on how stars of different masses evolve internally (e.g., with respect to T, P, etc.) that is worth reading is: 
<a href="http://adsabs.harvard.edu/abs/1967ARA%26A...5..571I">http://adsabs.harvard.edu/abs/1967ARA%26A...5..571I</a></p>

<p>A very interesting historical overview of the development of the Standard Solar Model:
<a href="http://arxiv.org/abs/astro-ph/0209080">http://arxiv.org/abs/astro-ph/0209080</a></p>

<p>This (admittedly dry) paper gives you a good idea of how well the 'standard' solar models estimate the internal properties of the Sun using helioseismology and neutrino measurements to help tie down their boundary conditions:
<a href="http://adsabs.harvard.edu/abs/1997PhRvL..78..171B">http://adsabs.harvard.edu/abs/1997PhRvL..78..171B</a>
The answer is that they match incredibly well (>0.2% error)</p>

<p>These were the least technical (but still academically published) references I could find.</p>

<p>Here is a comprehensive page on the state-of-the-art in solar modelling and measuring the internal Sun using Helioseismology:
<a href="http://www.sns.ias.edu/~jnb/Papers/Preprints/solarmodels.html">http://www.sns.ias.edu/~jnb/Papers/Preprints/solarmodels.html</a>
(highly technical)</p>

CC BY-SA 3.0
2013-09-26T20:04:05.897Z
2013-09-30T21:16:33.860Z
2013-09-30T21:16:33.860Z
pohuigin
<p>Thermonuclear fusion has nothing to do with the central temperature of the Sun. You can get a rough estimate of the temperature (with some necessary simplification) following this line of reasoning:</p>

<ol>
<li><p>The material of the Sun is an ideal, completely ionized, gas (all electrons are separated from nuclei);</p></li>
<li><p>This means that pressure of the gas is proportional to its temperature and to number of gas particles in unit volume;</p></li>
<li><p>Pressure in the center (innermost part) of the Sun must be large enough to support the weight of all the layers above;</p></li>
<li><p>If you suppose that the Sun is made only from hydrogen you get a central temperature of some 23 million degrees.</p></li>
</ol>

CC BY-SA 4.0
2019-05-24T06:14:12.020Z
I guess I understand what you are trying to say, but the first sentence is contentious. If there were no nuclear reactions the Sun, with its present radius, would have the same internal temperature. However, it would not stay like that and would become hotter and smaller.
ProfRob
CC BY-SA 4.0
2019-05-24T08:14:43.037Z
I think we do understand each other. My answer deals only with the hydrostatic equilibrum (with nondegenerate gas, temperature enters solution), that is gives answer to question how to prevent collapse of the Sun at scale of days. In fact, the Sun radiates - that is internal energy of gas leaks out into space, and the star must adjust accordingly on timescale of million years - in fact it shrinks and the central temperature increases. At some point the temperature is high enough to enable fusion and the star is stabilized (energy radiated is generated by fusion).
Leos Ondra
CC BY-SA 4.0
2019-05-24T08:22:37.333Z
Yes, so in that sense, nuclear fusion *does* determine the central temperature of the Sun, or at least prevent it getting even hotter. But I agree that you do not need to know about fusion to calculate the current central temperature of the Sun - given its current mass, radius and composition.
ProfRob
CC BY-SA 4.0
2019-05-24T08:27:29.893Z
I agree. Originally, I only wanted to emphasize the fusion is not the process which keeps the Sun interior hot (gravity and gas law are all we need). In fact, fusion prevents the interior from being *too* hot :-)
Leos Ondra
CC BY-SA 4.0
2019-05-23T18:32:50.050Z
2019-05-24T14:39:37.923Z
2019-05-24T14:39:37.923Z
Leos Ondra
<p>In general: you make models of the sun, and then you see which one agrees with all observations, and check which temperature this model predicts for the core.</p>

<p>A very simple model that gives a good approximation: fusion happens within a small volume in the core, and a part of the released energy is transported to the surface afterwards until it can escape as light. We know how much light the sun emits, and you can calculate the necessary temperature and density gradients inside that is required to transport this power and to keep the sun stable. Work from the surface inwards and you get an estimate for the core temperature.</p>

<p>Another nice approach is the fusion rate - this is known from the total power as well, and it can be compared to the fusion rate the sun would have at different temperatures.</p>

CC BY-SA 3.0
2014-07-20T18:28:53.190Z
2014-07-20T18:28:53.190Z
Murtuza Vadharia
<p>The composition can be determined by taking spectra. Additionally, the mass can be determined through dynamics. If you combine these two, under the assumption that the star is in a state of <a href="http://en.wikipedia.org/wiki/Hydrostatic_equilibrium" rel="nofollow noreferrer">hydrostatic equilibrium</a> (which means that the outward thermal pressure of the star due to fusion of hydrogen into helium is in balance with the inward tug of gravity), you can make statements about what the temperature and density <em>must</em> be in the core. You need high densities and high temperatures in order to fuse hydrogen into helium. </p>

<p>Remember what's happening: Temperatures are hot enough for hydrogen in the core to be completely ionized, meaning that in order to fuse these protons into helium nuclei, you need to overcome the electromagnetic repulsion as two protons come close (like charges repel). Below is a diagram of the process of one particular type of fusion (<a href="http://en.wikipedia.org/wiki/Proton%E2%80%93proton_chain_reaction" rel="nofollow noreferrer">Proton-proton chain reaction</a>).</p>

<p><img src="https://i.sstatic.net/4WpuY.png" alt="proton-proton">     </p>

<p>The other fusion reaction which occurs at the cores of stars is called the <a href="http://en.wikipedia.org/wiki/CNO_cycle" rel="nofollow noreferrer">carbon-nitrogen-oxygen</a> (CNO) cycle, and is the dominant source of energy for stars more massive than about 1.3 solar masses. Below shows this process.</p>

<p><img src="https://i.sstatic.net/5UMrk.png" alt="CNO"></p>

<p>Edit:<br>
Somebody pointed out that this doesn't actually answer the question at hand - which is true. Forgetting how to do some of the basic back of the envelope calculations myself (I admit, stellar astrophysics is definitely <em>not</em> my specialty), I've stumbled across a <em>very crude</em> and simple estimation of how to calculate the central pressure and temperature of the sun from. The <a href="http://burro.astr.cwru.edu/Academics/Astr221/StarPhys/estcent.html" rel="nofollow noreferrer">calculation</a> does however point out the correct values and what one would need to know in order to get the details correct.   </p>

CC BY-SA 3.0
2014-07-16T18:20:11.240Z
The temperature in the Sun is NOT sufficient to overcome the Coulomb barrier alone for Hydrogen fusion, but requires quantum tunneling.
Aaron
CC BY-SA 3.0
2013-09-30T22:30:59.757Z
This answer doesn't really answer the question as to how the temperature value of ~10^7 K is determined.
Guillochon
CC BY-SA 3.0
2013-09-30T23:26:23.520Z
@ Guillochon Yea, you're right. I was a bit too general. I'll try to update with a more specific answer.
astromax
CC BY-SA 3.0
2013-09-30T23:54:54.783Z
@Guillochon I've added a link. Feel free to modify/edit my answer if you have better information at hand.
astromax
CC BY-SA 3.0
2013-09-27T01:04:35.140Z
2014-07-16T16:38:18.537Z
2014-07-16T16:38:18.537Z
astromax
<p>It was estimated that the heat inside the core of the Sun inside around 15 000 000 °C - this value is extremely enormous. How did scientists estimate this value?</p>

CC BY-SA 3.0
2013-10-01T15:25:31.850Z
I just want to point out this very enlightening article about the difficulty in find a "simple" means of computing the Sun's structure (and thus central temperature), [Solar structure without computers](http://adsabs.harvard.edu/abs/1986AmJPh..54..354C). This is probably why you've yet to get an answer with a simple algebraic expression for the central temperature.
Guillochon
<the-sun><temperature><core>
How was the core temperature of the Sun estimated?
Zoltán Schmidt
# How was the core temperature of the Sun estimated?

(Asked by: username_0 on 2013-09-26)

It was estimated that the heat inside the core of the Sun inside around 15 000 000 °C - this value is extremely enormous. How did scientists estimate this value?

**Tags:** the-sun, temperature, core

> **Comments:**
> **username_1**: I just want to point out this very enlightening article about the difficulty in find a "simple" means of computing the Sun's structure (and thus central temperature), [Solar structure without computers](http://adsabs.harvard.edu/abs/1986AmJPh..54..354C). This is probably why you've yet to get an answer with a simple algebraic expression for the central temperature.  

---

## 4 answers

### Answer by username_6 on 2013-09-27. Score: 5 | Accepted answer

The composition can be determined by taking spectra. Additionally, the mass can be determined through dynamics. If you combine these two, under the assumption that the star is in a state of [hydrostatic equilibrium](http://en.wikipedia.org/wiki/Hydrostatic_equilibrium) (which means that the outward thermal pressure of the star due to fusion of hydrogen into helium is in balance with the inward tug of gravity), you can make statements about what the temperature and density *must* be in the core. You need high densities and high temperatures in order to fuse hydrogen into helium.

Remember what's happening: Temperatures are hot enough for hydrogen in the core to be completely ionized, meaning that in order to fuse these protons into helium nuclei, you need to overcome the electromagnetic repulsion as two protons come close (like charges repel). Below is a diagram of the process of one particular type of fusion ([Proton-proton chain reaction](http://en.wikipedia.org/wiki/Proton%E2%80%93proton_chain_reaction)).

![proton-proton](https://i.sstatic.net/4WpuY.png)

The other fusion reaction which occurs at the cores of stars is called the [carbon-nitrogen-oxygen](http://en.wikipedia.org/wiki/CNO_cycle) (CNO) cycle, and is the dominant source of energy for stars more massive than about 1.3 solar masses. Below shows this process.

![CNO](https://i.sstatic.net/5UMrk.png)

Edit:  
Somebody pointed out that this doesn't actually answer the question at hand - which is true. Forgetting how to do some of the basic back of the envelope calculations myself (I admit, stellar astrophysics is definitely *not* my specialty), I've stumbled across a *very crude* and simple estimation of how to calculate the central pressure and temperature of the sun from. The [calculation](http://burro.astr.cwru.edu/Academics/Astr221/StarPhys/estcent.html) does however point out the correct values and what one would need to know in order to get the details correct.

> **Comments:**
> **username_1**: This answer doesn't really answer the question as to how the temperature value of ~10^7 K is determined.  
> **username_6**: @ username_1 Yea, you're right. I was a bit too general. I'll try to update with a more specific answer.  
> **username_6**: @username_1 I've added a link. Feel free to modify/edit my answer if you have better information at hand.  
> **username_7**: The temperature in the Sun is NOT sufficient to overcome the Coulomb barrier alone for Hydrogen fusion, but requires quantum tunneling.  

---

### Answer by username_2 on 2013-09-26. Score: 15

Hydrodynamic models of the Sun allow one method of estimating its internal properties. To do this, the Mass, radius, surface temperature, and total luminosity (radiative energy emitted)/s of the Sun must be known (determined observationally). Making several assumptions, e.g., that the Sun behaves as a fluid and that local thermodynamic equilibrium applies, the stellar equations of state can be used. Numerical methods are applied to these equations to determine the internal properties of the Sun, such as its central temperature.

A great example for how to work this problem your self can be found in the undergraduate text, 'An Introduction to Modern Astrophysics' by Carroll and Ostlie (Section 10.5). The FORTRAN code to run your own stellar model is included in Appendix H.

A comprehensive review paper on how stars of different masses evolve internally (e.g., with respect to T, P, etc.) that is worth reading is:
<http://adsabs.harvard.edu/abs/1967ARA%26A...5..571I>

A very interesting historical overview of the development of the Standard Solar Model:
<http://arxiv.org/abs/astro-ph/0209080>

This (admittedly dry) paper gives you a good idea of how well the 'standard' solar models estimate the internal properties of the Sun using helioseismology and neutrino measurements to help tie down their boundary conditions:
<http://adsabs.harvard.edu/abs/1997PhRvL..78..171B>
The answer is that they match incredibly well (>0.2% error)

These were the least technical (but still academically published) references I could find.

Here is a comprehensive page on the state-of-the-art in solar modelling and measuring the internal Sun using Helioseismology:
<http://www.sns.ias.edu/~jnb/Papers/Preprints/solarmodels.html>
(highly technical)


---

### Answer by username_3 on 2019-05-23. Score: 3

Thermonuclear fusion has nothing to do with the central temperature of the Sun. You can get a rough estimate of the temperature (with some necessary simplification) following this line of reasoning:

1. The material of the Sun is an ideal, completely ionized, gas (all electrons are separated from nuclei);
2. This means that pressure of the gas is proportional to its temperature and to number of gas particles in unit volume;
3. Pressure in the center (innermost part) of the Sun must be large enough to support the weight of all the layers above;
4. If you suppose that the Sun is made only from hydrogen you get a central temperature of some 23 million degrees.

> **Comments:**
> **username_4**: I guess I understand what you are trying to say, but the first sentence is contentious. If there were no nuclear reactions the Sun, with its present radius, would have the same internal temperature. However, it would not stay like that and would become hotter and smaller.  
> **username_3**: I think we do understand each other. My answer deals only with the hydrostatic equilibrum (with nondegenerate gas, temperature enters solution), that is gives answer to question how to prevent collapse of the Sun at scale of days. In fact, the Sun radiates - that is internal energy of gas leaks out into space, and the star must adjust accordingly on timescale of million years - in fact it shrinks and the central temperature increases. At some point the temperature is high enough to enable fusion and the star is stabilized (energy radiated is generated by fusion).  
> **username_4**: Yes, so in that sense, nuclear fusion *does* determine the central temperature of the Sun, or at least prevent it getting even hotter. But I agree that you do not need to know about fusion to calculate the current central temperature of the Sun - given its current mass, radius and composition.  
> **username_3**: I agree. Originally, I only wanted to emphasize the fusion is not the process which keeps the Sun interior hot (gravity and gas law are all we need). In fact, fusion prevents the interior from being *too* hot :-)  

---

### Answer by username_5 on 2014-07-20. Score: 2

In general: you make models of the sun, and then you see which one agrees with all observations, and check which temperature this model predicts for the core.

A very simple model that gives a good approximation: fusion happens within a small volume in the core, and a part of the released energy is transported to the surface afterwards until it can escape as light. We know how much light the sun emits, and you can calculate the necessary temperature and density gradients inside that is required to transport this power and to keep the sun stable. Work from the surface inwards and you get an estimate for the core temperature.

Another nice approach is the fusion rate - this is known from the total power as well, and it can be compared to the fusion rate the sun would have at different temperatures.


---

