Difference between revisions of "Thermodynamical Properties of Elementary Particles"
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|+ |The Standard Model particles and their properties.== | |+ |The Standard Model particles and their properties.== | ||
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| − | === Problem | + | === Problem 7 === |
Generalize the results of the previous problem for the case when some $i$-components have temperature $T_i$ different from the CMB temperature $T$. | Generalize the results of the previous problem for the case when some $i$-components have temperature $T_i$ different from the CMB temperature $T$. | ||
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<div class="NavHead">solution</div> | <div class="NavHead">solution</div> | ||
<div style="width:100%;" class="NavContent"> | <div style="width:100%;" class="NavContent"> | ||
| − | <p style="text-align: left;"> </p> | + | <p style="text-align: left;"> |
| + | \[ | ||
| + | g^* = \sum\limits_{i = bosons} {g_i \left(\frac{T_i}{T} \right)^4 + \frac{7}{8}\sum\limits_{j = fermions}g_i \left( \frac{T_j}{T}\right)^4 | ||
| + | \] </p> | ||
</div> | </div> | ||
</div></div> | </div></div> | ||
| − | <div id=" | + | <div id="ter_6"></div> |
<div style="border: 1px solid #AAA; padding:5px;"> | <div style="border: 1px solid #AAA; padding:5px;"> | ||
| − | === Problem | + | === Problem 8 === |
| − | + | Find the effective number of internal degrees of freedom for the Standard Model particles at temperature $T>1TeV$. | |
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<div class="NavHead">solution</div> | <div class="NavHead">solution</div> | ||
<div style="width:100%;" class="NavContent"> | <div style="width:100%;" class="NavContent"> | ||
| − | <p style="text-align: left;"> | + | <p style="text-align: left;"> At temperature $1\, TeV$ all the Standard Model |
| + | particles are relativistic (see [[#tab:ter_sm|table]]). Therefore | ||
| + | \[ | ||
| + | g^* = 28 + \frac{7}{8} \times 90 = 106.75. | ||
| + | \] </p> | ||
</div> | </div> | ||
</div></div> | </div></div> | ||
Revision as of 18:07, 1 October 2012
In the mid-forties G.A.~Gamov proposed the idea
of the "hot" origin of the World. Therefore thermodynamics
was introduced into cosmology, and nuclear physics too.
Before him the science of the evolution of Universe
contained only dynamics and geometry of the World.
A.D.Chernin.
| Particles | Mass | Number of states | $g$ (particles and anti-particles) | |
|---|---|---|---|---|
| spin | color | |||
| Photon ($\gamma$) | 0 | 2 | 1 | 2 |
| $W^+,W^-$ | $80.4\, GeV$ | 3 | 1 | 6 |
| $Z$ | $91.2\,GeV$ | 3 | 1 | 3 |
| Gluon ($g$) | 0 | 2 | 8 | 16 |
| Higgs boson | $>114\, GeV$ | 1 | 1 | 1 |
| Bosons | 28 | |||
| $u,/,\bar{u}$ | $3\, MeV$ | 2 | 3 | 12 |
| $d,/,\bar{d}$ | $6\, MeV$ | 2 | 3 | 12 |
| $s,/,\bar{s}$ | $100\,MeV$ | 2 | 3 | 12 |
| $c,/,\bar{c}$ | $1.2\,GeV$ | 2 | 3 | 12 |
| $b,/,\bar{b}$ | $4.2\, GeV$ | 2 | 3 | 12 |
| $t,/,\bar{t}$ | $175\,GeV$ | 2 | 3 | 12 |
| $e^+,\,e^-$ | $0.511\, MeV $ | 2 | 1 | 4 |
| $\mu^+,\,\mu^-$ | $105.7\,MeV$ | 2 | 1 | 4 |
| $\tau^+,\,\tau^-$ | $1.777\, GeV$ | 2 | 1 | 4 |
| $\nu_e,\,\bar{\nu_e}$ | $<3\,eV$ | 1 | 1 | 2 |
| $\nu_\mu,\,\bar{\nu_\mu}$ | $<0.19\,MeV $ | 1 | 1 | 2 |
| $\nu_\tau,\,\bar{\nu_\tau}$ | $<18.2\, MeV $ | 1 | 1 | 2 |
| Fermions | 90 | |||
Contents
Problem 1
Find the energy and number densities for bosons and fermions in the relativistic limit.
The energy density equals to $$ \rho = \left\{ \begin{array}{c} \frac{\pi^2}{30}gT^4 \quad \; for\;bosons\\ \frac{7}{8}\frac{\pi^2}{30}gT^4 \quad for \;fermions \end{array} \right. $$ Here $g$ equals to the number of internal degrees of freedom for the particle. For photon (with spin $S=1$) $g=2$ due to absence of longitudinal polarization for the zero-mass particles. The number density is the following: \[ n = \left\{ \begin{array}{c} \frac{\zeta (3)}{\pi ^2 }gT^3 \quad \;for\;bosons \\ \frac{3} {4}\frac{\zeta (3)}{\pi ^2 }gT^3 \quad \; for\;fermions \end{array} \right. \] Here $\zeta (x)$ is the Riemann $\zeta$-function; $\zeta (3) \approx 1.202$.
Problem 2
Find the number densities and energy densities, normalized to the photon energy density at the same temperature, for neutrinos, electrons, positrons, pions and nucleons in the relativistic limit.
\[ \frac{n_i}{n_\gamma} = \left\{ \begin{gathered} \frac{1}{2}g_i \quad for\; bosons\\ \frac{3}{8}g_i \quad for\; fermions\\ \end{gathered} \right.;\quad \frac{\rho_i}{\rho_\gamma} = \left\{ \begin{gathered} \frac{1}{2}g_i \quad for\; bosons\\ \frac{7}{16}g_i \quad for\; fermions\\ \end{gathered} \right. \] \[ \begin{gathered} \left(\frac{n_i }{n_\gamma},\frac{\rho_i}{\rho_\gamma} \right)_{\nu_{\mu ,e}} = \left( \frac{3}{8},\frac{7}{16} \right);\;\;\left( \frac{n_i}{n_\gamma}, \frac{\rho_i}{\rho_\gamma} \right)_{e^\pm} = \left( \frac{3}{4},\frac{7}{8} \right);\\ \left( \frac{n_i}{n_\gamma},\frac{\rho_i}{\rho_\gamma} \right)_\pi = \left( \frac{1}{2},\frac{1}{2} \right);\;\;\left( \frac{n_i}{n_\gamma},\frac{\rho_i}{\rho_\gamma} \right)_{n,p} = \left( \frac{3}{4},\frac{7}{8} \right) \\ \end{gathered} \]
Problem 3
Calculate the average energy per particle in the relativistic and non-relativistic limits.
Average energy per particle reads$\left\langle \varepsilon \right\rangle = \rho /n$. For $T \gg m$ \[ \left\langle \varepsilon \right\rangle = \left\{ \begin{gathered} \frac{\pi ^2}{30\zeta (3)}T\quad \; for\; bosons\\ \frac{7\pi ^4}{180\zeta(3)}T\quad for\; fermions\\ \end{gathered} \right. \] In the non-relativistic limit $(T \ll m)$ one obtains the following: \[ \left\langle \varepsilon \right\rangle = m + \frac{3}{2}T \approx m \]
Problem 4
Find the number of internal degrees of freedom for a quark.
For quark one obtains the following: \[ g = 2(\, spin) \times 3(\, particle) \times 2(\, particles + \, antiparticle) = 12 \]
Problem 5
Find the entropy density for bosons end fermions with zero chemical potential.
In the considered case one gets: \[ s = \frac{\rho + p}{T};\quad p = \frac{1}{3}\rho \] Using the results of problem of the present Chapter one obtains the following: \[ s = \frac{2\pi ^2}{45}g^* T^3, \] where $g^* = 1$ for bosons and $g^* = 7/8$ for fermions.
Problem 6
Find the effective number of internal degrees of freedom for a mixture of relativistic bosons and fermions.
\[ \rho = \sum\limits_{i = bosons} g_i \frac{\pi^2}{30} T^4 + \sum\limits_{j = fermions} \frac{7}{8}g_j\frac{\pi^2}{30} T^4 \frac{\pi^2}{30}g^* T^4, \] where $g^* $ is the effective number of degrees of freedom: \[ g^* = \sum\limits_{i = bosons} g_i + \frac{7}{8}\sum\limits_{j = fermions}g_j. \]
Problem 7
Generalize the results of the previous problem for the case when some $i$-components have temperature $T_i$ different from the CMB temperature $T$.
\[ g^* = \sum\limits_{i = bosons} {g_i \left(\frac{T_i}{T} \right)^4 + \frac{7}{8}\sum\limits_{j = fermions}g_i \left( \frac{T_j}{T}\right)^4 \]
Problem 8
Find the effective number of internal degrees of freedom for the Standard Model particles at temperature $T>1TeV$.
At temperature $1\, TeV$ all the Standard Model particles are relativistic (see table). Therefore \[ g^* = 28 + \frac{7}{8} \times 90 = 106.75. \]
Problem 2
Problem 2
