<p>You can find a neat description and some examples of the effect <a href="http://www.jb.man.ac.uk/distance/frontiers/pulsars/section4.html" rel="nofollow noreferrer">here</a>. This is known as the <a href="http://astronomy.swin.edu.au/cms/astro/cosmos/p/Pulsar+Dispersion+Measure" rel="nofollow noreferrer">pulsar dispersion measure</a>. As you correctly say, waves with longer wavelength (lower energy photons) are delayed with respect to shorter wavelength radiation from the same phenomenon.</p>

<p>When electromagnetic waves travel through a plasma, they excite currents in the free charged particles. In such cases it can be shown (using Maxwell's equations) that the waves propagate with a relationship between their frequency <span class="math-container">$\omega$</span> and "wavenumber" <span class="math-container">$k = 2\pi/\lambda$</span> given by
<span class="math-container">$$\omega^2 = \omega_p^{2} + c^2k^2,$$</span>
where <span class="math-container">$\omega_p$</span> is known as the "plasma" frequency and equals <span class="math-container">$(n_e e^2/\epsilon_0 m_e)^{1/2}$</span> for the electrons in the plasma (i.e. it depends on the electron number density <span class="math-container">$n_e$</span>.).</p>

<p>Now, if you have a bunch of photons emitted as a pulse, the relevant velocity is the <a href="https://en.wikipedia.org/wiki/Group_velocity" rel="nofollow noreferrer">group velocity</a> given by <span class="math-container">$v_g=d\omega/dk$</span>. So
<span class="math-container">$$v_g = \frac{c^2 k}{(\omega_p^{2} +c^2 k^2)^{1/2}} = c\left(1 - \frac{\omega_p^2}{\omega^2}\right)^{1/2}$$</span></p>

<p>This converges to <span class="math-container">$c$</span> when the frequencies are high (wavelengths are short), but is slower when frequencies are low (wavelengths are long).</p>

<p>In terms of an intuitive physical picture, yes you could think that the refractive index is frequency dependent, but the difference here is that the reason for this dispersion is that waves travelling through a conductive medium are "lossy" - that is the currents induced also encounter resistivity and therefore the waves heat the plasma.</p>

CC BY-SA 4.0
2015-07-15T10:18:06.483Z
2019-12-14T10:37:06.223Z
2019-12-14T10:37:06.223Z
ProfRob
<p>Articles written about fast radio bursts describe the signal's short-wavelength components arriving before its longer-wavelength components, suggesting energy-dependent time delays in the interstellar medium (ex. <a href="http://www.scientificamerican.com/article/a-brilliant-flash-then-nothing-new-fast-radio-bursts-mystify-astronomers/" rel="noreferrer">http://www.scientificamerican.com/article/a-brilliant-flash-then-nothing-new-fast-radio-bursts-mystify-astronomers/</a>).</p>

<p><strong>Why are lower-energy signals slowed slightly more than higher-energy signals when passing through clouds of electrons?</strong> Also, <strong>how do we know about this slowing effect</strong> if it appears to be so small (what objects or events have exhibited the time difference)?</p>

<p>My first-order logic guessed that higher energy radiation is slowed more, remembering the mnemonic "<em>Blue bends best</em>" from optics. I assume these intergalactic clouds behave quite differently from a solid prism.</p>

<light><interstellar-medium><extinction>
Speed of light through the ISM and Wavelength
Sam
# Speed of light through the ISM and Wavelength

(Asked by: username_0 on 2015-07-14)

Articles written about fast radio bursts describe the signal's short-wavelength components arriving before its longer-wavelength components, suggesting energy-dependent time delays in the interstellar medium (ex. <http://www.scientificamerican.com/article/a-brilliant-flash-then-nothing-new-fast-radio-bursts-mystify-astronomers/>).

**Why are lower-energy signals slowed slightly more than higher-energy signals when passing through clouds of electrons?** Also, **how do we know about this slowing effect** if it appears to be so small (what objects or events have exhibited the time difference)?

My first-order logic guessed that higher energy radiation is slowed more, remembering the mnemonic "*Blue bends best*" from optics. I assume these intergalactic clouds behave quite differently from a solid prism.

**Tags:** light, interstellar-medium, extinction


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## 1 answers

### Answer by username_1 on 2015-07-15. Score: 6 | Accepted answer

You can find a neat description and some examples of the effect [here](http://www.jb.man.ac.uk/distance/frontiers/pulsars/section4.html). This is known as the [pulsar dispersion measure](http://astronomy.swin.edu.au/cms/astro/cosmos/p/Pulsar+Dispersion+Measure). As you correctly say, waves with longer wavelength (lower energy photons) are delayed with respect to shorter wavelength radiation from the same phenomenon.

When electromagnetic waves travel through a plasma, they excite currents in the free charged particles. In such cases it can be shown (using Maxwell's equations) that the waves propagate with a relationship between their frequency $\omega$ and "wavenumber" $k = 2\pi/\lambda$ given by
$$\omega^2 = \omega\_p^{2} + c^2k^2,$$
where $\omega\_p$ is known as the "plasma" frequency and equals $(n\_e e^2/\epsilon\_0 m\_e)^{1/2}$ for the electrons in the plasma (i.e. it depends on the electron number density $n\_e$.).

Now, if you have a bunch of photons emitted as a pulse, the relevant velocity is the [group velocity](https://en.wikipedia.org/wiki/Group_velocity) given by $v\_g=d\omega/dk$. So
$$v\_g = \frac{c^2 k}{(\omega\_p^{2} +c^2 k^2)^{1/2}} = c\left(1 - \frac{\omega\_p^2}{\omega^2}\right)^{1/2}$$

This converges to $c$ when the frequencies are high (wavelengths are short), but is slower when frequencies are low (wavelengths are long).

In terms of an intuitive physical picture, yes you could think that the refractive index is frequency dependent, but the difference here is that the reason for this dispersion is that waves travelling through a conductive medium are "lossy" - that is the currents induced also encounter resistivity and therefore the waves heat the plasma.


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