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An introduction to the science of cosmology

Derek Raine, E.G. Thomas

Chapter 9

Structure - all with Video Answers

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Chapter Questions

05:48

Problem 1

Solve equation (9.9) in the general case $R=t^n$. Show that perturbations are frozen-in once the Universe becomes curvature dominated (i.e. once matter density is negligible compared to the curvature term in the Friedmann equation).

Nick Johnson
Nick Johnson
Numerade Educator
02:19

Problem 2

Derive equation (9.9).

Sarah Lewites
Sarah Lewites
Numerade Educator
06:44

Problem 3

Show that for a sphere of radius $\lambda_{\mathrm{J}} / 2$ the free-fall collapse time is of order the hydrodynamical timescale $\lambda / c_{\mathrm{s}}$ and the gravitational energy equals the thermal energy.

Umar Sohail Qureshi
Umar Sohail Qureshi
Numerade Educator

Problem 4

(a) Show that the mass inside the Hubble sphere $M_{\mathrm{H}}$ grows as $R^{3 / 2}$ in a matter-dominated model. Find the corresponding rate of growth in the radiation-dominated case.
(b) Perturbation $\delta \rho / \rho$ grow proportional to $R$ in the matter-dominated case and proportional to $R^2$ in the radiation-dominated case. For perturbations
$(\delta \rho / \rho)_t$ outside the horizon at time $t$ show that in both radiation-dominated and matter-dominated models
$$
\left(\frac{\delta \rho}{\rho}\right)_t=M_{\mathrm{H}}^{-2 / 3}\left(\frac{\delta \rho}{\rho}\right)_{\mathrm{H}} .
$$

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05:48

Problem 5

At early times the curvature of space becomes large. Show that nevertheless at early times the horizon scale is much smaller than the radius of curvature h. Thus the curvature is insignificant within the horizon and Newtonian mechanics is applicable on this scale.

Nick Johnson
Nick Johnson
Numerade Educator

Problem 6

Observations of clusters gives a total matter density $\Omega_{\mathrm{M}} \simeq 0.3$. At the same time observation of the microwave background indicates a flat Universe $\Omega_0=1$. There must, therefore, be another source of mass energy that does not cluster to make up the difference, the dark energy $\Omega_{\mathrm{d}}$ (now) $\simeq 0.7$. This mass density cannot have been dominant in the past otherwise it would have prevented the formation of structure, so it must grow with time relative to the matter density. Use local energy conservation and the equation of state $P=w \rho c^2$ to show that, at time $t$,
$$
\rho_{\mathrm{d}} R^{3(\beta+1)}=\text { constant, }
$$
where $\beta=P /\left(\rho c^2\right)$. By considering the ratio $\Omega_{\mathrm{d}} / \Omega_{\mathrm{m}}$ deduce that the pressure of the dark energy must be negative. (This makes the vacuum energy or quintessence a candidate for the dark energy.)

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02:19

Problem 7

Show that the free-streaming length scale for relativistic particles in a radiation-dominated model between time $t=0$ and $t=t_{\mathrm{nt}}$ when the particles become non-relativistic is of order,
$$
\lambda_{\mathrm{fs}} \sim 2 \frac{t_{\mathrm{nr}}}{R_{\mathrm{nr}}},
$$
where $R_{\mathrm{nr}}=R\left(t_{\mathrm{nr}}\right)$. Deduce that $\lambda_{\mathrm{fs}} \sim 10\left(\Omega_{\mathrm{p}} h^2\right)^{-1}\left(T_{\mathrm{p}} / T\right)^4$ Mpc where $\Omega_{\mathrm{p}}$ is the contribution of this particle species to the density and $T_{\mathrm{p}}$ the temperature of the species (which differs from the radiation temperature $T$ because the particles are decoupled; see Kolb and Turner 1990 p 352).

Keshav Singh
Keshav Singh
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