<p>The expansion of the universe is described by a <a href="https://en.wikipedia.org/wiki/Scale_factor_(cosmology)" rel="nofollow noreferrer">scale factor</a> that we normally call <span class="math-container">$a(t)$</span>. We take the scale factor to be equal to one right now, so if <span class="math-container">$a(t)$</span> is less than one that means the universe has contracted while if <span class="math-container">$a(t)$</span> is greater than one the universe has expanded.</p>

<p>General relativity allows us to calculate how the scale factor depends on time. If you're interested I do this in the question <a href="https://physics.stackexchange.com/questions/136056/how-does-the-hubble-parameter-change-with-the-age-of-the-universe">How does the Hubble parameter change with the age of the universe?</a> on the Physics SE. This is what the results look like:</p>

<p><a href="https://i.sstatic.net/lWUhz.gif" rel="nofollow noreferrer"><img src="https://i.sstatic.net/lWUhz.gif" alt="Scale factor"></a></p>

<p>The point of this is that the CMB temperature is directly related to the scale factor so if we can calculate how the scale factor has changed with time then we can calculate the current CMB temperature.</p>

<p>But the way the scale factor changes with time depends on the density of matter and energy in the universe. Specifically it depends on how much light, matter (normal and dark) and dark energy is present. The matter/energy density could in principle have any values, that is there is no fundamental principle in physics that specifies what the densities of the of the various types of matter and energy have to be.</p>

<p>Our current best measurements of the matter/energy density come from the <a href="https://en.wikipedia.org/wiki/Planck_(spacecraft)" rel="nofollow noreferrer">Planck experiment</a>, and they suggest the total density has a value close to the <a href="http://astronomy.swin.edu.au/cosmos/C/Critical+Density" rel="nofollow noreferrer">critical density</a>. This density gives us the form of the scale factor that I drew above, and it gives us the CMB temperature of 2.7K. If the density were lower than critical we would get a lower CMB temperature and if the density were higher than critical we get a higher CMB temperature. So the answer to your question is that the CMB temperature is not uniquely determined and it could be higher or lower. Ultimately the CMB temperature is an experimental parameter that we have to determine by making experimental measurements.</p>

<p>But we should note that there are excellent reasons why we would expect the matter/energy density to be equal to the critical density, so we would expect the CMB temperature to be what we observe. If the CMB temperature were different by a factor of ten that would be hard to explain theoretically.</p>

<p>Finally we should note that there are other independent constraints of the form of the scale factor function. Rob Jeffries describes some of these <a href="https://astronomy.stackexchange.com/a/30550/10687">in his answer</a> so I won't go through them again here, but for example the ratio of hydrogen to helium depends on how quickly <span class="math-container">$a(t)$</span> increased after the Big Bang. If the scale factor had increased significantly faster or more slowly it would have changed the hydrogen to helium ratio and we'd be able to measure this change.</p>

CC BY-SA 4.0
2019-04-19T09:32:37.697Z
See below John. I think there are constraints based on timescales.
ProfRob
CC BY-SA 4.0
2019-04-19T10:20:01.177Z
@RobJeffries good point! :-)
John Rennie
CC BY-SA 4.0
2019-04-19T09:15:37.617Z
2019-04-20T04:03:24.790Z
2019-04-20T04:03:24.790Z
John Rennie
<p>Yes, I think it is a constraint, but don't think I can tell you how different it could be from 2.73 K to cause a problem.</p>

<p>The CMB tells us that the universe was once much hotter (<span class="math-container">$&gt;3000$</span> K), so that hydrogen nuclei and electrons had sufficient kinetic energies to remain uncombined. In the big-bang model, the universe expands and cools, then at temperatures just below this the protons
and electrons combine to form atoms that are almost transparent to the blackbody radiation that filled the universe before that. This radiation is then redshifts by the cosmological expansion and we still see it today as microwaves.</p>

<p>In the big-bang model, the temperature of the universe scales as <span class="math-container">$(1+z)^{-1}$</span>, where <span class="math-container">$z$</span> is the redshift corresponding to a particular look back time. That we see the CMB at 2.73 K now, means it occurred at <span class="math-container">$z=1100$</span>. Your question amounts to - would it matter if this were <span class="math-container">$z=110$</span> or <span class="math-container">$z=11000$</span>?</p>

<p>It's less complicated to deal with the lower of these possibilities. At <span class="math-container">$z&lt;3400$</span>, the energy density of the universe is matter dominated, and the scale factor <span class="math-container">$a \simeq (t/t_0)^{2/3}$</span>, where <span class="math-container">$t_0$</span> is the age of the universe and <span class="math-container">$a(t_0)=1$</span>. Since <span class="math-container">$1+z = a^{-1}$</span>, this means the connection between age and redshift is
<span class="math-container">$$ t(z) \simeq t_0 (1+z)^{-3/2}$$</span></p>

<p>If the CMB was formed at <span class="math-container">$z=1100$</span> this would be 370,000 years after the big bang (using the usual accepted cosmological parameters and an age of the universe of 13.7 billion years<span class="math-container">$^1$</span>). If instead we use <span class="math-container">$z=110$</span>, the CMB formed about 14 <em>million</em> years after the big bang.</p>

<p>That in itself is not a problem. We are just changing the expansion rate of the universe to match the redshift of the CMB and demanding this occurs just below 3000 K.</p>

<p>But this alters the temperature versus time relationship at all later and earlier times. How might this affect some other cosmological observations?</p>

<p>I think one area where the change in timescales would be hugely important is in primordial nucleosynthesis. By slowing down (or speeding up) the expansion rate, one allows an order of magnitude more (or less) time for nuclear reactions to take place.</p>

<p>An example: The neutron to proton ratio in the early universe freezes out at 1/6, but neutron decay with a half-life of 15 minutes, reduces the final ratio to 1/7 during the window of time available to nuclear reactions. If this window is made much bigger, the ratio will decrease further, if it is made much smaller the ratio will remain at 1/6.</p>

<p>Almost all of those neutrons end up in helium nuclei, so the primordial He abundance would vary between 10 H atoms per He atom through to something considerably bigger. The primordial He abundance is known to better than 1%, and it is around 12 H atoms per He atom. i.e. There was just enough time when primordial nuclear reactions were taking place for <em>some</em> of the free neutrons to decay, but not all. <strong>This would certainly seem to rule out order of magnitude changes in the CMB temperature.</strong></p>

<p>I may add to this as other things occur to me. There is likely another constraint based on the observed formation redshift of the first stars and the epoch of reionization.</p>

CC BY-SA 4.0
2019-04-19T11:34:36.887Z
You are saying that in your opinion the measured temperature of the cosmic microwave background radiation in itself does not contribute much to the empirical verification of the big bang model, because you can change some untestable parameters of the model, the rate of expansion, and still keep for instance the stated age of the universe? The CMB temperature together with the experimentally determined abundance of primordial He sets some constraints that forces the measured CMB temperature to be close to 2.7 K in order for the Big Bang model to hold?
Agerhell
CC BY-SA 4.0
2019-04-19T13:44:28.727Z
@Agerhell That would be my position at the moment. TBH, I am still thinking. This is a good question.
ProfRob
CC BY-SA 4.0
2019-04-19T16:59:48.350Z
It's a complex model, and there's room for some adjustment of the constants, but far from unlimited adjustment if you want to retain consistency with observation. Besides the CMB temperature and the neutron/proton ratio, the CMB irregularity spectrum, the observed location of galaxies in space, the precise ratios of various isotopes, and the distribution of supernovae all also constrain the model, so that tweaking the temperature by a factor of ten almost certainly make it inconsistent.
Mark Olson
CC BY-SA 4.0
2019-04-19T09:31:05.527Z
2019-04-19T13:47:37.067Z
2019-04-19T13:47:37.067Z
ProfRob
<p>I'd say it doesn't care all that much,  but that 27 degrees Kelvin is a step too far.</p>

<p>See the 1965 NASA csomic times article <a href="https://imagine.gsfc.nasa.gov/educators/programs/cosmictimes/online_edition/1965/hiss.html" rel="nofollow noreferrer">big hiss missed by others</a>. You can read how Andrei Doroshkevic and Igor Novikov published a Big Bang study in 1964 saying the remaining heat would now be between 1 and 10 degrees Kelvin. They proposed the use of the Holmdel horn measurements made in 1961 by Edward Ohm, who <em>“had already identified in his data what seemed to be a 3.3 degrees Kelvin background radiation”</em>. The article also says <em>“Ten years ago Émile Le Roux reported a microwave background radiation of 3 degrees Kelvin, plus or minus 2 degrees at the Nançay Radio Observatory”</em>. And this: <em>“In 1957 it was Tigran Shmaonov who nearly made the discovery. He reported measuring background temperature of 4 degrees Kelvin, give or take 3 degrees”</em>.</p>

<p>Of course, everybody knows about the famous back-to-back papers to the Astrophysical Journal in July 1965. They were <a href="http://adsabs.harvard.edu/abs/1965ApJ...142..419P" rel="nofollow noreferrer">A Measurement of Excess Antenna Temperature at 4080 Mc/s</a> by Penzias and Wilson, and <a href="http://adsabs.harvard.edu/abs/1965ApJ...142..414D" rel="nofollow noreferrer">Cosmic Black-Body Radiation</a> by Dicke, Peebles, Roll, and Wilkinson. What people don't generally know is that Dicke et al were talking about <em>"a closed universe, oscillating all the time"</em>. So according to them, the evidence for the <a href="https://en.wikipedia.org/wiki/Big_Bounce" rel="nofollow noreferrer">Big Bounce</a> had been found! </p>

<p>Personally I don't see any way by which the universe can ever contract. So I think the Big Bounce is a non-starter. However even though I'm 110% sure that the universe is expanding, I'm not happy with inflation or creation ex nihilo. So I think you're right to question the <a href="https://en.wikipedia.org/wiki/Big_Bang" rel="nofollow noreferrer">Big Bang</a>. The $64,0000 question is this: <em>what banged?</em> </p>

CC BY-SA 4.0
2019-04-19T13:10:37.130Z
110%? Think you'r a bit oversure on expansion. The theory looks good but there is no direct evidence. I asked. One could expect expansion to affect perspective but the early universe is too different to compare. Small chance the red shift is a direct property of the universe without expansion. For another $64,000 how about: Who nicked the anti-matter? The BB isn't that much an improvement on an admission that something happened but dunno exactly what or why.
Blame
CC BY-SA 4.0
2019-04-19T16:23:09.237Z
@Blame: See the Wikipedia [stress-energy tensor](https://en.wikipedia.org/wiki/Stress%E2%80%93energy_tensor) article and note the energy-pressure diagonal. I'm sure about the expansion because I'm confident GR is right, and it treats space as some kind of gin-clear ghostly elastic solid that has a pressure of sorts. The universe is like some squeezed-down stress ball when you open your fist. What I can't explain is why Einstein didn't predict the expanding universe. As for the antimatter, I have an opinion on that. See [this](http://physicsdetective.com/the-mystery-of-the-missing-antimatter/).
John Duffield
CC BY-SA 4.0
2019-04-19T20:40:40.290Z
Um.. will check that stress-energy thingy later when I feel less of the stress bit. That other article? Not buying it. Particles come in pairs and our universe got bilked out of half of em. Redefining the batch we got as bits from both teams solves nowt. It's just poor linguistics to re-use the terms matter & anti-matter for what is a new way of selecting which belongs to which team.
Blame
CC BY-SA 4.0
2019-04-20T07:33:56.527Z
@Blame : the important point to note is that the baryon asymmetry is matched by the lepton asymmetry, and there is no surplus of either protons or electrons. The poor linguistics is in using the term antimatter for both particles and combinations of particles.
John Duffield
CC BY-SA 4.0
2019-04-19T09:26:41.320Z
2019-04-19T09:31:59.420Z
2019-04-19T09:31:59.420Z
John Duffield
<p>The Big Bang is a proposed answer to the beginning of the universe, and the <a href="https://en.wikipedia.org/wiki/Cosmic_microwave_background" rel="nofollow noreferrer">Cosmic Microwave Background</a> or CMB is a central part of the evidence for it.</p>

<p>Now suppose the measurement returned a different value than 2.7K.</p>

<p>What if it were 0.27K or 27K?  Would the Big Bang theory still work with a few minor adjustments or is the specific temperature of 2.7K critical evidence that the theory works?</p>

<p>Edit: I have removed a paragraph which was not mine asking about small changes in temperature. It is a fundamentally different question. I am more interested in how firm the evidence for the BB theory is, not its details. At least for this question. 
However if uhoh who seems to have done the editing thinks it a fair question, I would certainly welcome it - in another post. </p>

CC BY-SA 4.0
2019-04-19T04:28:34.300Z
I was about to vote to close your question as asking for answers that were "primarily opinion based" until I read the last sentence. *That is an interesting question, so I'm going to clean up the stream of consciousness "sharing" in the beginning and keep the core of your question. Feel free to edit further.
uhoh
CC BY-SA 4.0
2019-04-19T08:00:25.130Z
The only thing I know is that in parallel to the finding of Wilson & Penzias a background of the right T was predicted.  When the two groups became aware of the counterpart results, they papers were submitted to the same journal where they appeared as companion letters.
Alchimista
CC BY-SA 4.0
2019-04-19T14:52:10.607Z
One of the primary predictions of the Big Bang theory is that the very distant universe would be markedly different from the local universe (denser, no hi-metallicity stars, rapid star formation, smaller galaxies).  The Hubble deep field observations showed that these predictions were correct.  This is a confirmation independent of the CMB.  There are multiple independent lines of evidence that only fit together nicely when a big bang is there to explain it all.
antlersoft
CC BY-SA 4.0
2019-04-20T08:00:03.380Z
The two papers about CMB prediction and finding are free access. I can't find them now but I "stumbled" on them just last week, following the links to the M87 BH series of papers. So they should be in the same Journal or perhaps a sister one.
Alchimista
CC BY-SA 4.0
2019-04-20T08:08:21.097Z
Here an anticipation, giving about 5 K. https://thecuriousastronomer.files.wordpress.com/2015/07/img_0290.jpg
Alchimista
CC BY-SA 4.0
2019-04-20T10:37:14.650Z
And correcting my use of the word "parallel" in previous comment https://physicstoday.scitation.org/doi/full/10.1063/PT.3.2859 a view from Alpher himself.
Alchimista
<cosmology><cosmic-microwave-background>
cosmic-microwave-background - 2.7 degrees but does the Big Bang care?
Blame
# cosmic-microwave-background - 2.7 degrees but does the Big Bang care?

(Asked by: username_0 on 2019-04-18)

The Big Bang is a proposed answer to the beginning of the universe, and the [Cosmic Microwave Background](https://en.wikipedia.org/wiki/Cosmic_microwave_background) or CMB is a central part of the evidence for it.

Now suppose the measurement returned a different value than 2.7K.

What if it were 0.27K or 27K? Would the Big Bang theory still work with a few minor adjustments or is the specific temperature of 2.7K critical evidence that the theory works?

Edit: I have removed a paragraph which was not mine asking about small changes in temperature. It is a fundamentally different question. I am more interested in how firm the evidence for the BB theory is, not its details. At least for this question.
However if username_1 who seems to have done the editing thinks it a fair question, I would certainly welcome it - in another post.

**Tags:** cosmology, cosmic-microwave-background

> **Comments:**
> **username_1**: I was about to vote to close your question as asking for answers that were "primarily opinion based" until I read the last sentence. *That is an interesting question, so I'm going to clean up the stream of consciousness "sharing" in the beginning and keep the core of your question. Feel free to edit further.  
> **username_2**: The only thing I know is that in parallel to the finding of Wilson & Penzias a background of the right T was predicted.  When the two groups became aware of the counterpart results, they papers were submitted to the same journal where they appeared as companion letters.  
> **username_3**: One of the primary predictions of the Big Bang theory is that the very distant universe would be markedly different from the local universe (denser, no hi-metallicity stars, rapid star formation, smaller galaxies).  The Hubble deep field observations showed that these predictions were correct.  This is a confirmation independent of the CMB.  There are multiple independent lines of evidence that only fit together nicely when a big bang is there to explain it all.  
> **username_2**: The two papers about CMB prediction and finding are free access. I can't find them now but I "stumbled" on them just last week, following the links to the M87 BH series of papers. So they should be in the same Journal or perhaps a sister one.  
> **username_2**: Here an anticipation, giving about 5 K. https://thecuriousastronomer.files.wordpress.com/2015/07/img_0290.jpg  
> **username_2**: And correcting my use of the word "parallel" in previous comment https://physicstoday.scitation.org/doi/full/10.1063/PT.3.2859 a view from Alpher himself.  

---

## 3 answers

### Answer by username_4 on 2019-04-19. Score: 4

The expansion of the universe is described by a [scale factor](https://en.wikipedia.org/wiki/Scale_factor_(cosmology)) that we normally call $a(t)$. We take the scale factor to be equal to one right now, so if $a(t)$ is less than one that means the universe has contracted while if $a(t)$ is greater than one the universe has expanded.

General relativity allows us to calculate how the scale factor depends on time. If you're interested I do this in the question [How does the Hubble parameter change with the age of the universe?](https://physics.stackexchange.com/questions/136056/how-does-the-hubble-parameter-change-with-the-age-of-the-universe) on the Physics SE. This is what the results look like:

[![Scale factor](https://i.sstatic.net/lWUhz.gif)](https://i.sstatic.net/lWUhz.gif)

The point of this is that the CMB temperature is directly related to the scale factor so if we can calculate how the scale factor has changed with time then we can calculate the current CMB temperature.

But the way the scale factor changes with time depends on the density of matter and energy in the universe. Specifically it depends on how much light, matter (normal and dark) and dark energy is present. The matter/energy density could in principle have any values, that is there is no fundamental principle in physics that specifies what the densities of the of the various types of matter and energy have to be.

Our current best measurements of the matter/energy density come from the [Planck experiment](https://en.wikipedia.org/wiki/Planck_(spacecraft)), and they suggest the total density has a value close to the [critical density](http://astronomy.swin.edu.au/cosmos/C/Critical+Density). This density gives us the form of the scale factor that I drew above, and it gives us the CMB temperature of 2.7K. If the density were lower than critical we would get a lower CMB temperature and if the density were higher than critical we get a higher CMB temperature. So the answer to your question is that the CMB temperature is not uniquely determined and it could be higher or lower. Ultimately the CMB temperature is an experimental parameter that we have to determine by making experimental measurements.

But we should note that there are excellent reasons why we would expect the matter/energy density to be equal to the critical density, so we would expect the CMB temperature to be what we observe. If the CMB temperature were different by a factor of ten that would be hard to explain theoretically.

Finally we should note that there are other independent constraints of the form of the scale factor function. Rob Jeffries describes some of these [in his answer](https://astronomy.stackexchange.com/a/30550/10687) so I won't go through them again here, but for example the ratio of hydrogen to helium depends on how quickly $a(t)$ increased after the Big Bang. If the scale factor had increased significantly faster or more slowly it would have changed the hydrogen to helium ratio and we'd be able to measure this change.

> **Comments:**
> **username_5**: See below username_4. I think there are constraints based on timescales.  
> **username_4**: @RobJeffries good point! :-)  

---

### Answer by username_5 on 2019-04-19. Score: 4

Yes, I think it is a constraint, but don't think I can tell you how different it could be from 2.73 K to cause a problem.

The CMB tells us that the universe was once much hotter ($>3000$ K), so that hydrogen nuclei and electrons had sufficient kinetic energies to remain uncombined. In the big-bang model, the universe expands and cools, then at temperatures just below this the protons
and electrons combine to form atoms that are almost transparent to the blackbody radiation that filled the universe before that. This radiation is then redshifts by the cosmological expansion and we still see it today as microwaves.

In the big-bang model, the temperature of the universe scales as $(1+z)^{-1}$, where $z$ is the redshift corresponding to a particular look back time. That we see the CMB at 2.73 K now, means it occurred at $z=1100$. Your question amounts to - would it matter if this were $z=110$ or $z=11000$?

It's less complicated to deal with the lower of these possibilities. At $z<3400$, the energy density of the universe is matter dominated, and the scale factor $a \simeq (t/t\_0)^{2/3}$, where $t\_0$ is the age of the universe and $a(t\_0)=1$. Since $1+z = a^{-1}$, this means the connection between age and redshift is
$$ t(z) \simeq t\_0 (1+z)^{-3/2}$$

If the CMB was formed at $z=1100$ this would be 370,000 years after the big bang (using the usual accepted cosmological parameters and an age of the universe of 13.7 billion years$^1$). If instead we use $z=110$, the CMB formed about 14 *million* years after the big bang.

That in itself is not a problem. We are just changing the expansion rate of the universe to match the redshift of the CMB and demanding this occurs just below 3000 K.

But this alters the temperature versus time relationship at all later and earlier times. How might this affect some other cosmological observations?

I think one area where the change in timescales would be hugely important is in primordial nucleosynthesis. By slowing down (or speeding up) the expansion rate, one allows an order of magnitude more (or less) time for nuclear reactions to take place.

An example: The neutron to proton ratio in the early universe freezes out at 1/6, but neutron decay with a half-life of 15 minutes, reduces the final ratio to 1/7 during the window of time available to nuclear reactions. If this window is made much bigger, the ratio will decrease further, if it is made much smaller the ratio will remain at 1/6.

Almost all of those neutrons end up in helium nuclei, so the primordial He abundance would vary between 10 H atoms per He atom through to something considerably bigger. The primordial He abundance is known to better than 1%, and it is around 12 H atoms per He atom. i.e. There was just enough time when primordial nuclear reactions were taking place for *some* of the free neutrons to decay, but not all. **This would certainly seem to rule out order of magnitude changes in the CMB temperature.**

I may add to this as other things occur to me. There is likely another constraint based on the observed formation redshift of the first stars and the epoch of reionization.

> **Comments:**
> **username_6**: You are saying that in your opinion the measured temperature of the cosmic microwave background radiation in itself does not contribute much to the empirical verification of the big bang model, because you can change some untestable parameters of the model, the rate of expansion, and still keep for instance the stated age of the universe? The CMB temperature together with the experimentally determined abundance of primordial He sets some constraints that forces the measured CMB temperature to be close to 2.7 K in order for the Big Bang model to hold?  
> **username_5**: @username_6 That would be my position at the moment. TBH, I am still thinking. This is a good question.  
> **username_7**: It's a complex model, and there's room for some adjustment of the constants, but far from unlimited adjustment if you want to retain consistency with observation. Besides the CMB temperature and the neutron/proton ratio, the CMB irregularity spectrum, the observed location of galaxies in space, the precise ratios of various isotopes, and the distribution of supernovae all also constrain the model, so that tweaking the temperature by a factor of ten almost certainly make it inconsistent.  

---

### Answer by username_8 on 2019-04-19. Score: -1

I'd say it doesn't care all that much, but that 27 degrees Kelvin is a step too far.

See the 1965 NASA csomic times article [big hiss missed by others](https://imagine.gsfc.nasa.gov/educators/programs/cosmictimes/online_edition/1965/hiss.html). You can read how Andrei Doroshkevic and Igor Novikov published a Big Bang study in 1964 saying the remaining heat would now be between 1 and 10 degrees Kelvin. They proposed the use of the Holmdel horn measurements made in 1961 by Edward Ohm, who *“had already identified in his data what seemed to be a 3.3 degrees Kelvin background radiation”*. The article also says *“Ten years ago Émile Le Roux reported a microwave background radiation of 3 degrees Kelvin, plus or minus 2 degrees at the Nançay Radio Observatory”*. And this: *“In 1957 it was Tigran Shmaonov who nearly made the discovery. He reported measuring background temperature of 4 degrees Kelvin, give or take 3 degrees”*.

Of course, everybody knows about the famous back-to-back papers to the Astrophysical Journal in July 1965. They were [A Measurement of Excess Antenna Temperature at 4080 Mc/s](http://adsabs.harvard.edu/abs/1965ApJ...142..419P) by Penzias and Wilson, and [Cosmic Black-Body Radiation](http://adsabs.harvard.edu/abs/1965ApJ...142..414D) by Dicke, Peebles, Roll, and Wilkinson. What people don't generally know is that Dicke et al were talking about *"a closed universe, oscillating all the time"*. So according to them, the evidence for the [Big Bounce](https://en.wikipedia.org/wiki/Big_Bounce) had been found!

Personally I don't see any way by which the universe can ever contract. So I think the Big Bounce is a non-starter. However even though I'm 110% sure that the universe is expanding, I'm not happy with inflation or creation ex nihilo. So I think you're right to question the [Big Bang](https://en.wikipedia.org/wiki/Big_Bang). The $64,0000 question is this: *what banged?*

> **Comments:**
> **username_0**: 110%? Think you'r a bit oversure on expansion. The theory looks good but there is no direct evidence. I asked. One could expect expansion to affect perspective but the early universe is too different to compare. Small chance the red shift is a direct property of the universe without expansion. For another $64,000 how about: Who nicked the anti-matter? The BB isn't that much an improvement on an admission that something happened but dunno exactly what or why.  
> **username_8**: @username_0: See the Wikipedia [stress-energy tensor](https://en.wikipedia.org/wiki/Stress%E2%80%93energy_tensor) article and note the energy-pressure diagonal. I'm sure about the expansion because I'm confident GR is right, and it treats space as some kind of gin-clear ghostly elastic solid that has a pressure of sorts. The universe is like some squeezed-down stress ball when you open your fist. What I can't explain is why Einstein didn't predict the expanding universe. As for the antimatter, I have an opinion on that. See [this](http://physicsdetective.com/the-mystery-of-the-missing-antimatter/).  
> **username_0**: Um.. will check that stress-energy thingy later when I feel less of the stress bit. That other article? Not buying it. Particles come in pairs and our universe got bilked out of half of em. Redefining the batch we got as bits from both teams solves nowt. It's just poor linguistics to re-use the terms matter & anti-matter for what is a new way of selecting which belongs to which team.  
> **username_8**: @username_0 : the important point to note is that the baryon asymmetry is matched by the lepton asymmetry, and there is no surplus of either protons or electrons. The poor linguistics is in using the term antimatter for both particles and combinations of particles.  

---

