<p>The question is compromised by saying that you allow arbitrarily perfect measurements.</p>

<p>If we have a bolometer that can measure the amount of flux from a star, at a distance that is known to arbitrary accuracy, with arbitrarily good spatial resolution, then what we do is measure the bolometric luminosity from a 1 m$^2$ area at the centre of the stellar disk. This flux is $\sigma T_{eff}^4$.</p>

<p>Now of course, stars do not have homogeneous atmospheres (spots, granulation, meridional flows, non-sphericity due to rotation...), so the result you would get would depend on exactly what 1 m$^2$ bit of atmosphere you were looking at. So, with my arbitrarily accurate instruments I would have to measure the luminosity from every 1 m$^2$ patch over the entire surface of the star. Each one would give me another estimate of $T_{eff}^4$; each would be somewhat different. That would be difficult, but the form of your question allows me to ignore those problems.</p>

<p>At this level of precision, the utility of a single $T_{eff}$ for the whole star is questionable, but if you wanted one then it would be the flux-weighted mean of all the above measurements, and as far as I can see one can <em>instantaneously</em> determine it to whatever accuracy you desire. Of course it will then vary if you have a variable star, and it will vary from point to point with time due to granulation; so the accuracy of the $T_{eff}$ could depend on how quickly and by how much it varies compared with how long it takes you to do your arbitrarily accurate measurements.</p>

<p>I think to get a better answer, you do need to specify some realistic observational constraints - such as (a) you cannot resolve the star at all, or (b) that you can resolve it, but observations can only take place from an earth-bound observatory (thus not allowing you to take flux measurements from the whole surface at once).</p>

<p>One thing occurs, is that in unresolved observations, even with an absolutely accurately measured luminosity (assuming isotropic radiation) there is still the issue of what radius to use. The radius at which the radiation escapes the star (at optical depth $\sim 2/3$) is ill-defined and wavelength dependent. An error bar of maybe tens of km is appropriate here, since atmospheres are 100-200 km "thick". For a solar-type star this would limit $T_{eff}$ accuracy to $\sim 0.1 K$ !</p>

CC BY-SA 3.0
2015-10-18T17:21:46.497Z
Dear Rob, I completely agree with your point, it is not possible to give one unique value for the stellar temperature, for indeed there are various kinds of imperfections going on: inhomogenieties, non-LTE, temperature variation over the photosphere,  stellar variability, you name it. However, with the present spectroscopy/stellar models the precision is such that these problems above may be typically omitted as non-significant. The question I am asking then is relatively well defined: until what precision in temperature measurements is it still meaningful to talk about stellar temperature.
Alexey Bobrick
CC BY-SA 3.0
2015-10-18T17:22:50.550Z
And more precisely, I would ideally like to know the number. Is 1K precision meaningless, or is it meaningless to talk about Teff already at precision of 100K, or... ?
Alexey Bobrick
CC BY-SA 3.0
2015-10-18T18:02:27.530Z
@AlexeyBobrick Teff is completely defined, whatever the complications of the atmosphere, so a number could always be errived at. I don't agree that current models are so inaccurate that inhomogeneities and 3D effects don't matter. They may be large and they may be systematic. e.g. I believe that extensive spots on M-dwarfs mean that their Teff is very significantly lower than estimated from colours/spectroscopy. The limiting uncertainty in Teff will come from a definition of the radius at which the radiation escapes. Edit  in progress.
ProfRob
CC BY-SA 3.0
2015-10-18T18:17:45.270Z
Yes, it is a very good point, that there also important systematic contributions. Still, again, the question really is about the magnitudes of the most relevant perturbing effects. Ideally, I would like to see a statement of the kind (this is made up): "For solar-like stars it doesn't make sense to talk about Teff up to precision better than 50K, because the convection causes a variability in the recovered Teff on the scales of a few hours."
Alexey Bobrick
CC BY-SA 3.0
2015-10-18T19:26:09.413Z
@AlexeyBobrick We may be able to discuss in person. I will be at Lund on 30th Oct.
ProfRob
CC BY-SA 3.0
2015-10-18T19:48:17.597Z
Which is indeed most peculiar and nice, I suppose your visit has something to do with the coming PhD defence there. Will gladly continue the discussion in person!
Alexey Bobrick
CC BY-SA 3.0
2015-10-18T15:43:53.480Z
2015-10-18T18:11:15.657Z
2015-10-18T18:11:15.657Z
ProfRob
<p>It is quite easy. In fact you do not need a bolometer. You just need to perform Intensity measurements in several parts of the spectrum, and then fit these to a theoretical black body spectrum. Three uses to be enough if it does not happen that you are measuring on a spike or valley in the spectrum caused by an emission or absorption line. The black body spectrum that best fits your measurements will give you <span class="math-container">$T_{eff}$</span>.</p>

CC BY-SA 3.0
2015-10-18T17:55:41.553Z
This only works if the star is a blackbody. Stars are not blackbodies. The method you propose is akin to the Infra red flux method, which although insensitive to, does require a model for the stellar spectrum.
ProfRob
CC BY-SA 3.0
2013-11-24T13:50:51.893Z
First off, part of the uncertainty of the temperature will come from the goodness of the fit (what will it be?). Secondly, do you mean spectrum over the whole disk, or just in the center? If it is the disc, you are measuring T of rather different layers, of it is the center, you are more subject to irregularities (by how much?). Finally, remember about stellar varibility, sunspots, etc. Given all this, no, it is not quite easy. There is a set of phenomena, which limit foundamentally the robustness of the definition of $T$. Main point of my question is - to what degree?
Alexey Bobrick
CC BY-SA 3.0
2013-11-24T20:01:54.010Z
It is quite easy, since for most stars out there we can not distinguish disc and atmosphere. All we see is a Airy disc of the whole of the star light.
Envite
CC BY-SA 3.0
2013-11-24T20:14:30.417Z
Perhaps, I should have stressed in the question, but I really mean that we are looking at the star with arbitrarily perfect instruments: with perfect resolution, sensitivity etc. When talking about the disc, because of limb darkening different parts of the disc correspond to different temperatures.
Alexey Bobrick
CC BY-SA 3.0
2013-11-25T02:16:07.253Z
With perfect instruments you would simply measure R with a perfect telescope and L with a perfect bolometer and apply the formula. No trouble in that.
Envite
CC BY-SA 3.0
2013-11-25T10:55:08.553Z
And how do you 'simply' measure R with a perfect telescope? Let me remind you that R is dependent on $\lambda$, and that the stars are not spheres, nor are they isotropic and contant in time. You can argue, that these are all small effects, but it is the value of the errors from them that I am looking for. Whether the definition of $T_{eff}$ is model dependent up to $10 \textrm{K}$, or whether it is $1\textrm{K}$, or some $10^{-4} \textrm{K}$.
Alexey Bobrick
CC BY-SA 3.0
2013-11-25T11:56:45.533Z
Once you say you are using a perfect bolometer, you need to use the widest possible R, that is, the one that encompasses all the emitted radiation of any wavelenght you are measuring with the bolometer. And if you want something better, remember that 4piR2 is just the sphere surface, so if you want better precision than that of a spherical formula you'd use L=S\sigma T_{eff}^4
Envite
CC BY-SA 3.0
2013-11-25T15:08:57.600Z
Yes, but then $R$ becomes arbitrary. Which one should we use?
Alexey Bobrick
CC BY-SA 3.0
2013-11-25T15:19:52.873Z
None. You use S as a defined surface for which you find an L. Please note that what you actually measure at Earth is not L but I.
Envite
CC BY-SA 3.0
2013-11-25T16:09:37.130Z
Well. $L$ does not depend on radius/size/shape of the surface, while $S$ does. So, which $S$ to use?
Alexey Bobrick
CC BY-SA 4.0
2013-11-24T13:37:41.127Z
2021-03-25T15:54:08.310Z
2021-03-25T15:54:08.310Z
Envite
<p>This is a question about the basics of astronomy, which I have never happened to see a good discussion for. It is about how well would we be able to measure effective temperature of a star, if we had any arbitrarily perfect measurement devices.</p>

<p>Here is some context. Canonical definition of $T_{\textrm{eff}}$ of a star is based on its bolometric luminosity $L$ (total electromagnetic energy radiated by the star per unit time) and its photospheric radius R (radius, at which the optical depth at a given wavelength is equal to unity). This way, the definition specifies  $T_{\textrm{eff}}$ through $L=4\pi \sigma R^2 T_{\textrm{eff}}^4$, where $\sigma$ is Stefan-Boltzmann constant. </p>

<p>The definition clearly alludes to black-body law. Many stars, including our own Sun, have a spectrum that does not follow it. For this reason, one often talks about another effective temperature, which is the temperature of stellar material at photospheric radius, and which can be determined by examining stellar spectrum. There are a few more complications to that, but let's put them aside.</p>

<p>Determining  $T_{\textrm{eff}}$ is extremely important in characterising stars, therefore there exists a variety of methods of measuring it, and naturally researchers strive for obtaining the best possible precision.</p>

<p>Hence, the question: <strong>How well can one in principle measure $T_{\textrm{eff}}$, if one could have arbitrarily perfect instruments?</strong> </p>

<p>Edit: <strong>I would like to see a quantitative estimate in your answer. Is the best possible precision for $T_{\textrm{eff}}$ of order $10\textrm{K}$, or is it $1\textrm{K}$, or some $10^{-4}\textrm{K}$, or can we measure it arbitrarily well?</strong></p>

<p>Here are just a few sources of uncertainty/arbitrariness: convection in stars, dependence of photospheric radius on wavelength, limb darkening, stellar variability, to name a few.</p>

<p>I would encourage the answers to be in the format "Source of uncertainty" - "Simple derivation" - "Estimate of the effect". If there are more than a few estimates, I will add a summary of them in the question or in a separate reply. Please, also feel free to edit the question if you might like to.</p>

<spectroscopy><stellar-atmospheres><radiative-transfer><stellar-structure>
How well can we in principle determine $T_{\textrm{eff}}$ of a star?
Alexey Bobrick
# How well can we in principle determine $T_{\textrm{eff}}$ of a star?

(Asked by: username_0 on 2013-11-23)

This is a question about the basics of astronomy, which I have never happened to see a good discussion for. It is about how well would we be able to measure effective temperature of a star, if we had any arbitrarily perfect measurement devices.

Here is some context. Canonical definition of $T\_{\textrm{eff}}$ of a star is based on its bolometric luminosity $L$ (total electromagnetic energy radiated by the star per unit time) and its photospheric radius R (radius, at which the optical depth at a given wavelength is equal to unity). This way, the definition specifies $T\_{\textrm{eff}}$ through $L=4\pi \sigma R^2 T\_{\textrm{eff}}^4$, where $\sigma$ is Stefan-Boltzmann constant.

The definition clearly alludes to black-body law. Many stars, including our own Sun, have a spectrum that does not follow it. For this reason, one often talks about another effective temperature, which is the temperature of stellar material at photospheric radius, and which can be determined by examining stellar spectrum. There are a few more complications to that, but let's put them aside.

Determining $T\_{\textrm{eff}}$ is extremely important in characterising stars, therefore there exists a variety of methods of measuring it, and naturally researchers strive for obtaining the best possible precision.

Hence, the question: **How well can one in principle measure $T\_{\textrm{eff}}$, if one could have arbitrarily perfect instruments?**

Edit: **I would like to see a quantitative estimate in your answer. Is the best possible precision for $T\_{\textrm{eff}}$ of order $10\textrm{K}$, or is it $1\textrm{K}$, or some $10^{-4}\textrm{K}$, or can we measure it arbitrarily well?**

Here are just a few sources of uncertainty/arbitrariness: convection in stars, dependence of photospheric radius on wavelength, limb darkening, stellar variability, to name a few.

I would encourage the answers to be in the format "Source of uncertainty" - "Simple derivation" - "Estimate of the effect". If there are more than a few estimates, I will add a summary of them in the question or in a separate reply. Please, also feel free to edit the question if you might like to.

**Tags:** spectroscopy, stellar-atmospheres, radiative-transfer, stellar-structure

---

## 2 answers

### Answer by username_1 on 2015-10-18. Score: 3

The question is compromised by saying that you allow arbitrarily perfect measurements.

If we have a bolometer that can measure the amount of flux from a star, at a distance that is known to arbitrary accuracy, with arbitrarily good spatial resolution, then what we do is measure the bolometric luminosity from a 1 m$^2$ area at the centre of the stellar disk. This flux is $\sigma T\_{eff}^4$.

Now of course, stars do not have homogeneous atmospheres (spots, granulation, meridional flows, non-sphericity due to rotation...), so the result you would get would depend on exactly what 1 m$^2$ bit of atmosphere you were looking at. So, with my arbitrarily accurate instruments I would have to measure the luminosity from every 1 m$^2$ patch over the entire surface of the star. Each one would give me another estimate of $T\_{eff}^4$; each would be somewhat different. That would be difficult, but the form of your question allows me to ignore those problems.

At this level of precision, the utility of a single $T\_{eff}$ for the whole star is questionable, but if you wanted one then it would be the flux-weighted mean of all the above measurements, and as far as I can see one can *instantaneously* determine it to whatever accuracy you desire. Of course it will then vary if you have a variable star, and it will vary from point to point with time due to granulation; so the accuracy of the $T\_{eff}$ could depend on how quickly and by how much it varies compared with how long it takes you to do your arbitrarily accurate measurements.

I think to get a better answer, you do need to specify some realistic observational constraints - such as (a) you cannot resolve the star at all, or (b) that you can resolve it, but observations can only take place from an earth-bound observatory (thus not allowing you to take flux measurements from the whole surface at once).

One thing occurs, is that in unresolved observations, even with an absolutely accurately measured luminosity (assuming isotropic radiation) there is still the issue of what radius to use. The radius at which the radiation escapes the star (at optical depth $\sim 2/3$) is ill-defined and wavelength dependent. An error bar of maybe tens of km is appropriate here, since atmospheres are 100-200 km "thick". For a solar-type star this would limit $T\_{eff}$ accuracy to $\sim 0.1 K$ !

> **Comments:**
> **username_0**: Dear Rob, I completely agree with your point, it is not possible to give one unique value for the stellar temperature, for indeed there are various kinds of imperfections going on: inhomogenieties, non-LTE, temperature variation over the photosphere,  stellar variability, you name it. However, with the present spectroscopy/stellar models the precision is such that these problems above may be typically omitted as non-significant. The question I am asking then is relatively well defined: until what precision in temperature measurements is it still meaningful to talk about stellar temperature.  
> **username_0**: And more precisely, I would ideally like to know the number. Is 1K precision meaningless, or is it meaningless to talk about Teff already at precision of 100K, or... ?  
> **username_1**: @AlexeyBobrick Teff is completely defined, whatever the complications of the atmosphere, so a number could always be errived at. I don't agree that current models are so inaccurate that inhomogeneities and 3D effects don't matter. They may be large and they may be systematic. e.g. I believe that extensive spots on M-dwarfs mean that their Teff is very significantly lower than estimated from colours/spectroscopy. The limiting uncertainty in Teff will come from a definition of the radius at which the radiation escapes. Edit  in progress.  
> **username_0**: Yes, it is a very good point, that there also important systematic contributions. Still, again, the question really is about the magnitudes of the most relevant perturbing effects. Ideally, I would like to see a statement of the kind (this is made up): "For solar-like stars it doesn't make sense to talk about Teff up to precision better than 50K, because the convection causes a variability in the recovered Teff on the scales of a few hours."  
> **username_1**: @AlexeyBobrick We may be able to discuss in person. I will be at Lund on 30th Oct.  
> **username_0**: Which is indeed most peculiar and nice, I suppose your visit has something to do with the coming PhD defence there. Will gladly continue the discussion in person!  

---

### Answer by username_2 on 2013-11-24. Score: 1

It is quite easy. In fact you do not need a bolometer. You just need to perform Intensity measurements in several parts of the spectrum, and then fit these to a theoretical black body spectrum. Three uses to be enough if it does not happen that you are measuring on a spike or valley in the spectrum caused by an emission or absorption line. The black body spectrum that best fits your measurements will give you $T\_{eff}$.

> **Comments:**
> **username_0**: First off, part of the uncertainty of the temperature will come from the goodness of the fit (what will it be?). Secondly, do you mean spectrum over the whole disk, or just in the center? If it is the disc, you are measuring T of rather different layers, of it is the center, you are more subject to irregularities (by how much?). Finally, remember about stellar varibility, sunspots, etc. Given all this, no, it is not quite easy. There is a set of phenomena, which limit foundamentally the robustness of the definition of $T$. Main point of my question is - to what degree?  
> **username_2**: It is quite easy, since for most stars out there we can not distinguish disc and atmosphere. All we see is a Airy disc of the whole of the star light.  
> **username_0**: Perhaps, I should have stressed in the question, but I really mean that we are looking at the star with arbitrarily perfect instruments: with perfect resolution, sensitivity etc. When talking about the disc, because of limb darkening different parts of the disc correspond to different temperatures.  
> **username_2**: With perfect instruments you would simply measure R with a perfect telescope and L with a perfect bolometer and apply the formula. No trouble in that.  
> **username_0**: And how do you 'simply' measure R with a perfect telescope? Let me remind you that R is dependent on $\lambda$, and that the stars are not spheres, nor are they isotropic and contant in time. You can argue, that these are all small effects, but it is the value of the errors from them that I am looking for. Whether the definition of $T_{eff}$ is model dependent up to $10 \textrm{K}$, or whether it is $1\textrm{K}$, or some $10^{-4} \textrm{K}$.  
> **username_2**: Once you say you are using a perfect bolometer, you need to use the widest possible R, that is, the one that encompasses all the emitted radiation of any wavelenght you are measuring with the bolometer. And if you want something better, remember that 4piR2 is just the sphere surface, so if you want better precision than that of a spherical formula you'd use L=S\sigma T_{eff}^4  
> **username_0**: Yes, but then $R$ becomes arbitrary. Which one should we use?  
> **username_2**: None. You use S as a defined surface for which you find an L. Please note that what you actually measure at Earth is not L but I.  
> **username_0**: Well. $L$ does not depend on radius/size/shape of the surface, while $S$ does. So, which $S$ to use?  
> **username_1**: This only works if the star is a blackbody. Stars are not blackbodies. The method you propose is akin to the Infra red flux method, which although insensitive to, does require a model for the stellar spectrum.  

---

