I have been considering a generalisation of the cosmological process involved in computing the temperature of the cosmic neutrino background.

It is well-known that (simplistically) this temperature $T_{\nu}$ differs from the temperature of the CMB $T_{\gamma}$ by a factor of $(4/11)^{1/3}$ due to the fact that shortly after neutrino-decoupling at 0.8 MeV, electrons and positrons annihilate and dump energy to the photon plasma which is still at equilibrium, while leaving the temperature of the decoupled neutrinos constant, as they no longer interact with the plasma.

I was wondering what would happen if the neutrinos decoupled before any particles became non-relativistic ($T > 100$ GeV) such that they had to go through all of the 'annihilation' processes as follows: top quarks, Higgs + W + Z, bottom quarks, charm quarks, tau leptons, (QCD phase transition), pions, muons, and electrons. Specifically, I am wondering what happens for the annihilation processes which are not of the form

\begin{equation} X^+ + X^- \rightarrow \gamma \gamma, \end{equation}

such as the annihilation of Higgs, W bosons and Z bosons, and what happens at the QCD phase transition (between tau annihilation and pion annihilation). These processes do change the number of relativistic degrees of freedom in entropy, so if we just used the conservation of entropy to compute the temperature we would treat them the same way as the other processes. However do these processes actually dump energy to the plasma? I can't see why they would.


All the particles that annihilate or decay as they become non-relativistic, heat the photon bath. A decaying particle, like the Higgs, also heats the photon bath by decaying to lighter particles, giving those particles alot of energy.

In general, if the neutrinos had decoupled at a temperature $T_\text{dc}$, the temperature of the neutrinos would, at any later time, be given by: \begin{equation} T_\nu = \left(\frac{g_{*S}(T)}{g_{*S}(T_\text{dc})}\right)^{1/3}T, \end{equation} where the effective number of relativistic degrees of freedom, $g_{*S}$, is given by \begin{equation} g_{*S} = \sum_{\text{bosons}}^{\text{relativistic}} g_i \left(\frac{T_i}{T}\right)^3 + \frac{7}{8} \sum_{\text{fermions}}^{\text{relativistic}} g_i \left(\frac{T_i}{T}\right)^3. \end{equation}

| cite | improve this answer | |
  • $\begingroup$ What about QCD phase transition? This changes the types of particles present so that the number of degrees of freedom changes, but doesn't contain any annihilations. Shouldn't this mean that we should apply your first equation twice: once before QCD and once after? $\endgroup$ – Orca May 28 '16 at 14:41
  • 1
    $\begingroup$ Yes, the evolution during the QCD phase transition will be complicated, but as you say, if you want the temperature afterwards you just apply the formula. But I disagree that there are no annihilations in this process, virtually all the protons and antiprotons annihilate to leave a tiny ($10^{-10}$)remnant of protons (because of a tiny initial asymmetry between particles and antiparticles). $\endgroup$ – Ihle May 28 '16 at 14:59
  • 1
    $\begingroup$ I was also wondering what your source for this was (and other related things)? I haven't really found a good source for cosmological thermal history. $\endgroup$ – Orca May 28 '16 at 19:21
  • 1
    $\begingroup$ @Orca: The de facto classic for such things is 'The Early Universe' by Kolb & Turner. Refer section 5.2 of the book to answer your original question. $\endgroup$ – Siva Jun 2 '16 at 16:12

Your Answer

By clicking “Post Your Answer”, you agree to our terms of service, privacy policy and cookie policy

Not the answer you're looking for? Browse other questions tagged or ask your own question.