<p>My attempts at a short answer failed, so here is my best shot at an explanation.</p>
<p>When you look at what the photon-baryon plasma does in the dark matter background, you will bump into an equation that is <em>almost</em> the equation for a harmonic oscillator, but it contains a time dependent quantity <span class="math-container">$\chi = \frac{3\rho_B}{4\rho_\gamma}$</span> that spoils the fun. It is, however, possible to approximate the solution:
<span class="math-container">$$\Theta_k(\tau) + \Phi_k \approx A_k \cos\Big(k\int_0^\tau c_s(\tau')d\tau'\Big) - \chi\Phi_k$$</span>
where <span class="math-container">$\Theta$</span> is the temperature fluctuation <span class="math-container">$\delta T/T$</span> (in Fourier space), <span class="math-container">$\tau$</span> is the conformal time, <span class="math-container">$\Phi$</span> is the potential caused by dark matter and <span class="math-container">$c_s$</span> is the sound speed in the plasma. The observable quantity is <span class="math-container">$\Theta_{0k} = \Theta_k + \Phi_k$</span>. These are the intrinsic temperature fluctuations plus the background potential.
The prefactor <span class="math-container">$A_k$</span> is determined by evaluating this expression at <span class="math-container">$\tau = \tau_{LS}$</span>, the moment of last scattering. This then yields:
<span class="math-container">$$\Theta_{0k} = \frac{1}{3}(1 + 3\chi)\Phi_k\cos(k\lambda_s) - \chi\Phi_k $$</span>
with <span class="math-container">$\lambda_s = \int_0^{\tau_{LS}} c_s d\tau$</span> the sound horizon (i.e. the distance acoustic waves can travel in a certain amount of time). The quantity <span class="math-container">$\Theta_{0k}$</span> is called the monopole contribution to the CMB. The dipole contribution, that is due to the Doppler effect, is much smaller and I will not consider it here.</p>
<p>Let's take a look at an overdensity (<span class="math-container">$\Phi_k &lt; 0$</span>) and place our coordinate axes right in the middle of it. At the &quot;time of the Big Bang&quot;, <span class="math-container">$\tau = 0$</span> the monopole is <span class="math-container">$\Theta_{0k} = \frac{1}{3}\Phi_k &lt;0$</span>. The argument of the cosine is 0, so the cosine itself reaches its maximum value.
Half a period of the cosine later: <span class="math-container">$\Theta_{0k} = -\frac{1}{3}(1 + 6\chi)\Phi_k$</span>, which is a lot larger! In the standard cosmological model, <span class="math-container">$\Phi_k$</span> remains constant, so the only thing that could have gotten bigger is the intrinsic temperature fluctuation <span class="math-container">$\Theta$</span>. This temperature fluctuation is directly linked to the density fluctuations of the photons and baryons.</p>
<p>What happens intuitively is the following: the baryons love falling into dark matter potentials. Baryons are approximately pressureless, so nothing would impede them to do so if it weren't for the photons to which they are coupled before <span class="math-container">$\tau_{LS}$</span>. The photons are dragged down into the potential well by the baryons, which makes them hotter (photons do have pressure), so thermodynamics tells them to cool again by escaping the well. It's much harder to get out of a potential well than it is to fall into one, so the amplitudes of compression (<span class="math-container">$B$</span> and <span class="math-container">$\gamma$</span> falling into a well) and expansion (<span class="math-container">$\gamma$</span> pushing <span class="math-container">$B$</span> out of the well) are not equal.</p>
<p>Look again at the cosine at <span class="math-container">$\tau_{LS}$</span>. It will reach maximal compression when <span class="math-container">$k\lambda_s = (2n + 1)\pi$</span> for <span class="math-container">$n = 0, 1, 2...$</span>, which defines the wavenumbers of the fluctuations that reach maximal compression. It will reach maximal expansion when <span class="math-container">$k\lambda_s = 2n\pi$</span> for <span class="math-container">$n = 1, 2, 3...$</span>.</p>
<p>The first peak reaches maximal compression at last scattering. It is huge because it is least affected by Silk diffusion. It corresponds to a large angular scale (compared to the other peaks) because its wavelength is <span class="math-container">$\lambda = 2\lambda_s$</span> and is therefore the largest fluctuation.</p>
<p>And finally, I think you already found Wayne Hu's website, but here is the <a href="http://background.uchicago.edu/%7Ewhu/intermediate/gravity.html" rel="nofollow noreferrer">link to a gif</a> that shows you the oscillation of the baryon-photon plasma in a dark matter potential well.</p>

CC BY-SA 4.0
2021-01-09T14:11:45.080Z
2021-01-09T15:19:57.790Z
2021-01-09T15:19:57.790Z
theWrongAlice
<p>I have read up quite a bit on the CMB power spectrum, but one feature evades my understanding. The first peak is often referred to as the &quot;first compression peak&quot;, meaning that the plasma had time to compress exactly once. The way I imagine this is that we have a central overdensity, and then a ring of plasma around it which moves closer, i.e. the ring is being compressed. In the same vein I think of the second peak as corresponding to the ring being compressed and then rarefacted. But I don't see how this fits in with the power spectrum: the first peak corresponds to a <em>larger</em> separation between the center and the ring, while the second peak corresponds to a <em>smaller</em> separation. With the way I have described it, I believe it should be the other way around: compression should correspond to smaller scales, while rarefaction should correspond to larger scales.</p>
<p>What am I misunderstanding about this?
<a href="https://i.sstatic.net/mvb9G.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/mvb9G.png" alt="enter image description here" /></a></p>

<cosmic-microwave-background>
Understanding the angular peaks in the CMB power spectrum
Kristian
# Understanding the angular peaks in the CMB power spectrum

(Asked by: username_0 on 2021-01-08)

I have read up quite a bit on the CMB power spectrum, but one feature evades my understanding. The first peak is often referred to as the "first compression peak", meaning that the plasma had time to compress exactly once. The way I imagine this is that we have a central overdensity, and then a ring of plasma around it which moves closer, i.e. the ring is being compressed. In the same vein I think of the second peak as corresponding to the ring being compressed and then rarefacted. But I don't see how this fits in with the power spectrum: the first peak corresponds to a *larger* separation between the center and the ring, while the second peak corresponds to a *smaller* separation. With the way I have described it, I believe it should be the other way around: compression should correspond to smaller scales, while rarefaction should correspond to larger scales.

What am I misunderstanding about this?
[![enter image description here](https://i.sstatic.net/mvb9G.png)](https://i.sstatic.net/mvb9G.png)

**Tags:** cosmic-microwave-background


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## 1 answers

### Answer by username_1 on 2021-01-09. Score: 1 | Accepted answer

My attempts at a short answer failed, so here is my best shot at an explanation.

When you look at what the photon-baryon plasma does in the dark matter background, you will bump into an equation that is *almost* the equation for a harmonic oscillator, but it contains a time dependent quantity $\chi = \frac{3\rho\_B}{4\rho\_\gamma}$ that spoils the fun. It is, however, possible to approximate the solution:
$$\Theta\_k(\tau) + \Phi\_k \approx A\_k \cos\Big(k\int\_0^\tau c\_s(\tau')d\tau'\Big) - \chi\Phi\_k$$
where $\Theta$ is the temperature fluctuation $\delta T/T$ (in Fourier space), $\tau$ is the conformal time, $\Phi$ is the potential caused by dark matter and $c\_s$ is the sound speed in the plasma. The observable quantity is $\Theta\_{0k} = \Theta\_k + \Phi\_k$. These are the intrinsic temperature fluctuations plus the background potential.
The prefactor $A\_k$ is determined by evaluating this expression at $\tau = \tau\_{LS}$, the moment of last scattering. This then yields:
$$\Theta\_{0k} = \frac{1}{3}(1 + 3\chi)\Phi\_k\cos(k\lambda\_s) - \chi\Phi\_k $$
with $\lambda\_s = \int\_0^{\tau\_{LS}} c\_s d\tau$ the sound horizon (i.e. the distance acoustic waves can travel in a certain amount of time). The quantity $\Theta\_{0k}$ is called the monopole contribution to the CMB. The dipole contribution, that is due to the Doppler effect, is much smaller and I will not consider it here.

Let's take a look at an overdensity ($\Phi\_k < 0$) and place our coordinate axes right in the middle of it. At the "time of the Big Bang", $\tau = 0$ the monopole is $\Theta\_{0k} = \frac{1}{3}\Phi\_k <0$. The argument of the cosine is 0, so the cosine itself reaches its maximum value.
Half a period of the cosine later: $\Theta\_{0k} = -\frac{1}{3}(1 + 6\chi)\Phi\_k$, which is a lot larger! In the standard cosmological model, $\Phi\_k$ remains constant, so the only thing that could have gotten bigger is the intrinsic temperature fluctuation $\Theta$. This temperature fluctuation is directly linked to the density fluctuations of the photons and baryons.

What happens intuitively is the following: the baryons love falling into dark matter potentials. Baryons are approximately pressureless, so nothing would impede them to do so if it weren't for the photons to which they are coupled before $\tau\_{LS}$. The photons are dragged down into the potential well by the baryons, which makes them hotter (photons do have pressure), so thermodynamics tells them to cool again by escaping the well. It's much harder to get out of a potential well than it is to fall into one, so the amplitudes of compression ($B$ and $\gamma$ falling into a well) and expansion ($\gamma$ pushing $B$ out of the well) are not equal.

Look again at the cosine at $\tau\_{LS}$. It will reach maximal compression when $k\lambda\_s = (2n + 1)\pi$ for $n = 0, 1, 2...$, which defines the wavenumbers of the fluctuations that reach maximal compression. It will reach maximal expansion when $k\lambda\_s = 2n\pi$ for $n = 1, 2, 3...$.

The first peak reaches maximal compression at last scattering. It is huge because it is least affected by Silk diffusion. It corresponds to a large angular scale (compared to the other peaks) because its wavelength is $\lambda = 2\lambda\_s$ and is therefore the largest fluctuation.

And finally, I think you already found Wayne Hu's website, but here is the [link to a gif](http://background.uchicago.edu/%7Ewhu/intermediate/gravity.html) that shows you the oscillation of the baryon-photon plasma in a dark matter potential well.


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