Cosmology

Table of Contents

1. Hubble's Law

\[ v = Hr \] where \(v\) is the recession speed of a galaxy, and \(r\) is the distance from the Earth, \(H\) is the Hubble's constant.

It suggest that the universe is expanding.

2. Cosmological Principle

The universe is

  • Spatially homogeneous
  • Spatially isotropic

This let us assume, at large scale:

  • Universe has uniform mass density \(\rho\)
  • Universe has uniform pressue \(p\)
  • Universe can have a time-varying scale factor \(a(t)\)

3. Friedmann-Lemaître-Robertson-Walker Metric

  • FLRW Metric

\[ g_{\mu\nu} = \begin{bmatrix} 1 & 0 & 0 & 0 \\ 0 & -\dfrac{a(t)^{2}}{1 - kr^2} & 0 & 0 \\ 0 & 0 & -(a(t)r)^2 & 0 \\ 0 & 0 & 0 & -(a(t)r\sin \theta)^2 \end{bmatrix} \] where \(a(t)\) is the time-varying scale factor, \(k\) is the curvature of the universe: \(+1\) if spherical, \(0\) if flat, \(-1\) if hyperbolic. \(r\) is the normalized radial coordinate that varies from 0 to 1.

This metric is combination of three metric by reparameterization in the radial direction.

\begin{alignat*}{3} \text{elliptic}&: \ &g_{\mu\nu}(t, \chi, \theta, \phi) &= \begin{bmatrix} 1 & 0 & 0 & 0 \\ 0 & a(t)^2 & 0 & 0 \\ 0 & 0 & -(a(t)\sin\chi)^2 & 0 \\ 0 & 0 & 0 & -(a(t)\sin\chi\sin \theta)^2 \end{bmatrix}\quad &\stackrel{r = \sin\chi}{\longrightarrow}\ &g_{\mu\nu}\big|_{k=1}\\ \text{flat}&: \ &g_{\mu\nu}(t, \chi, \theta, \phi) &= \begin{bmatrix} 1 & 0 & 0 & 0 \\ 0 & a(t)^2 & 0 & 0 \\ 0 & 0 & -(a(t)\chi)^2 & 0 \\ 0 & 0 & 0 & -(a(t)\chi\sin \theta)^2 \end{bmatrix} \quad &\stackrel{r = \chi}{\longrightarrow}\ &g_{\mu\nu}\big|_{k=0}\\ \text{hyperbolic}&: \ &g_{\mu\nu}(t, \chi, \theta, \phi) &= \begin{bmatrix} 1 & 0 & 0 & 0 \\ 0 & a(t)^2 & 0 & 0 \\ 0 & 0 & -(a(t)\sinh\chi)^2 & 0 \\ 0 & 0 & 0 & -(a(t)\sinh\chi\sin \theta)^2 \end{bmatrix} \quad& \stackrel{r = \sinh\chi}{\longrightarrow}\ &g_{\mu\nu}\big|_{k=-1} \end{alignat*}

Spherical geometry has larger interior while hyperbolic geometry has smaller interior.

\(r\) is called the comoving reduced-circumference coordinate that is proportional to the circumference \(C\) at that point around the origin: \[ r = \frac{C}{2\pi a(t)}. \]

3.1. Connection Coefficients

All nonzero Christoffel symbols are listed.

\[ \Gamma^r_{tr}=\Gamma^r_{rt}=\frac{1}{c}\frac{\dot a}{a},\qquad \Gamma^\theta_{t\theta}=\Gamma^\theta_{\theta t}=\frac{1}{c}\frac{\dot a}{a},\qquad \Gamma^\phi_{t\phi}=\Gamma^\phi_{\phi t}=\frac{1}{c}\frac{\dot a}{a} \]

\[ \Gamma^t_{rr}=\frac{1}{c}\frac{a\dot a}{1-kr^2},\qquad \Gamma^t_{\theta\theta}=\frac{1}{c}a\dot a\, r^2,\qquad \Gamma^t_{\phi\phi}=\frac{1}{c}a\dot a\, r^2\sin^2\theta \] \[ \Gamma^r_{rr}=\frac{kr}{1-kr^2},\qquad \Gamma^r_{\theta\theta}=-r(1-kr^2),\qquad \Gamma^r_{\phi\phi}=-r(1-kr^2)\sin^2\theta \] \[ \Gamma^\theta_{\phi\phi}=-\sin\theta\cos\theta \]

\[ \Gamma^\theta_{r\theta}=\Gamma^\theta_{\theta r}=\frac{1}{r},\qquad \Gamma^\phi_{r\phi}=\Gamma^\phi_{\phi r}=\frac{1}{r} \] \[ \Gamma^\phi_{\theta\phi}=\Gamma^\phi_{\phi\theta}=\cot\theta \]

3.2. Ricci Tensor

Ricci tensor is diagonal tensor.

\[ R_{tt} = -\frac{3}{c^2}\frac{\ddot a}{a} \] \[ R_{rr} = \frac{1}{c^2}\frac{a\ddot a + 2\dot a^2 + 2kc^2}{1-kr^2} \] \[ R_{\theta\theta} = \frac{1}{c^2}r^2\left(a\ddot a + 2\dot a^2 + 2kc^2\right) \] \[ R_{\phi\phi} = \frac{1}{c^2}r^2\sin^2\theta\left(a\ddot a + 2\dot a^2 + 2kc^2\right) \]

The spatial components can also be written as \[ R_{ii} = \frac{1}{c^2}\left(a\ddot a + 2\dot a^2 + 2kc^2\right) \gamma_{ii} \] where \(\gamma_{ii} = - g_{ii}/a(t)^2\).

They add up to Ricci scalar \[ R = - \frac{6}{c^2} \frac{ a\ddot a + \dot a^2 + kc^2}{a^2}. \]

3.3. Comoving Coordinates

Worldline along constant space coordinates \(r, \theta, \phi\), is geodesic in FLRW metric. For this reason FLRW coordinates \(ct, r, \theta, \phi\) are called comoving coordinates.

3.4. Cosmological Redshift

The redshift as observed by comoving observer in cosmic rest frame depends on the scale factor: \[ \frac{f_o}{f_e} = \frac{a(t_e)}{a(t_o)} \] where \(f_o\) and \(t_o\) are the frequency and the time when the light is observed, and \(f_e\) and \(t_e\) are the frequency and the time when the light was emitted.

Quantity \(z\) is also defined: \[ 1+z := \frac{a(t_e)}{a(t_o)}. \]

4. Cosmic Rest Frame

Frame in which the large scale average momentum is zero, and the time coordinate of time scale \(a(t)\) is given in.

This frame is the one that has no observed Doppler shift in cosmic microwave background radiation. Frame at rest relative to CMB radiation.

The energy-momentum tensor for Friedmann equation is measured in this frame.

5. Horizons

5.1. Hubble Horizon

Boundary beyond which galaxies are moving away from Earth faster than light. \[ L_{H}(t) = \frac{c}{H(t)}. \] \(L\) indicates that it is proper length.

\(L_{Hh} \approx 14\, \mathrm{Gly}\)

5.2. Cosmic Event Horizon

The maximum comoving distance \(\Delta r\) a light beam emitted from Earth can travel. \[ r_{eh} = \int_{t_{\text{now}}}^{\infty} \frac{1}{a(t)} \dd{ct}. \] The proper length is then \(L_{eh} = a(t) r_{eh}\).

If Hubble parameter \(H(t)\) is constant for all time, Hubble horizon and event horizon are the same.

\(L_{eh} \approx 16\, \mathrm{Gly}\)

5.3. Particle Horizon

The maximum distance \(\Delta r\) a light beam has travelled since the beginning of the univrse. The region within particle horizon is called the observable universe. \[ r_{ph} = \int_0^{t_{\text{now}}} \frac{1}{a(t)} \dd{ct}. \]

\(L_{ph} \approx 45\, \mathrm{Gly}\)

6. Mass-Energy Content

6.1. Equation of State

The simplest equation of state is chosen for the matter and radiation in the universe: \[ p = w\rho c^2 \] assuming that it is barotropic fluid.

6.2. Perfect Fluid

Matter and energy are assumed to be perfect fluid. If \(w = 0\), we get a energy-momentum tensor for dust-like matter \[ T^{\mu}{}_{\nu} = \begin{bmatrix} \rho c^2 & 0 & 0 & 0 \\ 0 & 0 & 0 & 0 \\ 0 & 0 & 0 & 0 \\ 0 & 0 & 0 & 0 \end{bmatrix}. \]

The energy-momentum tensor for electromagnetic radiation is given by \[ T^{\mu\nu} = \frac{1}{\mu_0} \left( F^{\mu\alpha}F^{\nu}{}_{\alpha} - \frac{1}{4}g^{\mu\nu}F^{\alpha\beta}F_{\alpha\beta} \right). \] This tensor has zero trace, therefore we require \(w = 1/3\), in order to describe electromagnetic radiation.

If \(w=-1\) we find that \[ T_{\mu\nu} = \rho c^2 g_{\mu\nu} \] which resembles the cosmological constant term \(\Lambda g_{\mu\nu}\) in Einstein field equation, that describing the thing that accelerates the expansion of the universe.

6.3. Critical Density

The energy density \(\rho_c\) at which the curvature \(k = 0\).

We can express current energy density \(\rho\) in terms of critical density using density parameter \(\Omega_{\rm M/R}\): \[ \Omega_{\rm M/R} := \frac{\rho}{\rho_c}. \] \(\rm M/R\) subscript means that the energy density is considering the matter and radiation.

Critical density in flat universe \(k=0\) with no cosmological constant \(\Lambda=0\): \[ \rho_c = \frac{3H^2}{8\pi G}, \] where \(H\) is the Hubble parameter.

The first Friedmann equation can be rewritten as \[ 1 = \frac{8\pi G \rho}{3 H^2} + \frac{\Lambda c^2}{3 H^2} - \frac{k c^2}{a^2 H^2} \] in which we can define each term to be density parameter \(\Omega_{\rm M/R}\), dark energy parameter \(\Omega_{\Lambda}\), and curvature parameter \(\Omega_{\rm k}\): \[ 1 = \Omega_{\rm M/R} + \Omega_{\Lambda} + \Omega_{\rm k}. \]

7. Friedmann Equations

The equation is derived from Einstein field equation with FLRW metric on LHS, and a model for mass-energy content on RHS.

7.1. First Friedmann Equation

From the 00-component of the Einstein field equation:

\begin{align*} & R_{00} - \frac{1}{2}R g_{00} - \Lambda g_{00} = \frac{8\pi G}{c^4}T_{00} \\ \implies &\frac{\dot{a}^2 + kc^2}{a^2} = \frac{8\pi G\rho + \Lambda c^2}{3}. \end{align*}

7.2. Second Friedmann Equation

From the trace of the Einstein field equation:

\begin{align*} & R_{\mu\nu} g^{\mu\nu} - \frac{1}{2}R g_{\mu\nu} g^{\mu\nu} - \Lambda g_{\mu\nu} g^{\mu\nu} = \frac{8 \pi G}{c^4} T_{\mu\nu} g^{\mu\nu} \\ \implies &-R - 4\Lambda = \frac{8\pi G}{c^4}T \\ \implies & \frac{\ddot{a}}{a} + \frac{\dot{a}^2 + kc^2}{a^2} - \frac{2}{3}\Lambda c^2 = \frac{4\pi G}{3} \left( \rho - 3 \frac{p}{c^2}\right) \\ \end{align*}

and replacing with the first Friedmann equation, \[ \implies \frac{\ddot{a}}{a} = \frac{1}{3} \Lambda c^2 - \frac{4\pi G}{3} \left( \rho + \frac{p}{c^2} \right). \]

7.3. Third Friedmann Equation

  • The name is not widely accepted

Obtained by taking derivative of first Friedmann equation, and substituting the second Friedmann equation in. \[ \dot{\rho} = -3 \frac{\dot{a}}{a} \left( \rho + \frac{p}{c^2}\right). \]

The same equation can be obtained by assuming that the universe expands adiabatically, or using the local conservation of energy-momentum.

7.4. Energy Density

The energy density can be expressed in terms of the scaling factor, by combining equation of state with the third Friedmann equation: \[ \rho(a) = K a^{-3(1+w)}. \]

8. de Sitter Universe

It is assumed that:

  • \(\rho = 0\)
  • \(p = 0\)
  • \(k = 0\)

\[ a(t) = a_0 \exp \left( \sqrt{\frac{\Lambda c^2}{3}}t \right) = a_0 e^{Ht} \] where \(H\) is the constant Hubble parameter. This universe is dominated by cosmological constant, or dark energy.

The curvature can also assumed to be \(1\) or \(-1\).

9. Anti-de Sitter Universe

Empty universe with negative cosmological constant \(\Lambda < 0\) only admit real solution for \(a(t)\) when \(k = -1\).

\[ a(t) = \sqrt{-\frac{3}{\Lambda}} \sin \left( \sqrt{-\frac{\Lambda c^2}{3}} t + C_1 \right) \]

10. de Sitter Space

  • Homogeneous and isotropic universe for both space and time

Empty spacetime with positive curvature is called the de Sitter space, while empty spacetime with negative curvature is called the anti-de Sitter space. In contrast the empty spacetime with zero curvature is called the Minkowksi space.

de Sitter space is 4D space modelled in 5D: \[ x^2 + y^2 + z^2 + w^2 - q^2 = R^2, \] and similarly for anti-de Sitter space: \[ x^2 + y^2 + z^2 - w^2 - q^2 = -R^2. \]

11. Dark Matter

11.1. Self-Interacting Dark Matter

  • SIDM

Hypothesis that dark matter interact with itself, in addition to gravity.

11.2. MOdified Newtonian Dynamics

  • MOND

Hypothesis that the gravity changes its strength based on length scale.

11.3. Bullet Cluster

It is two colliding clusters of galaxies, where the distribution mass obtained based on the gravitational lensing is outpacing the movement of the intergalactic gas which are colliding in the interface of the collision and stagnating behind.

It is known that the majority of the mass comes from the gas. But, the mass distribution aligns with the distribution of galaxies which did not interact with each other much. This suggest the existence of non-interacting matter.

12. Dark Energy

12.1. Cosmological Constant

The cosmological constant \(\Lambda\) in the Einstein field equation is may be the result of dark energy, as the equation can be rewritten in trace-reversed form that indicates \(\Lambda\) can be some kind of source of curvature: \[ R_{\mu\nu} = \frac{8\pi G}{c^4} \left( T_{\mu\nu} - \frac{1}{2}\left( T + \frac{c^4}{4\pi G}\Lambda\right) g_{\mu\nu} \right). \]

13. Standard Cosmology

With no cosmological constant \(\Lambda = 0\), \[ \Omega_{\rm M/R} - 1 = \Omega_{\rm k} \] and the sign of LHS determine the curvature \(k\).

By the first Friedmann equation, the curvature is the ultimate factor that determines the evolution of the universe, as the energy term will diminish as scale factor increases:

  • \(k=-1\): Open (expand forever)
  • \(k=0\): Flat (reach a maximum)
  • \(k=+1\): Closed (shrink onto itself)

When cosmological constant is less than zero \(\Lambda < 0\), the second Friedmann equation tells us that the scale factor will always decelerate, leading to eventual Big crunch regardless of other parameters.

When cosmological constant is greater than zero \(\Lambda > 0\),

  • \(k= 0\) or \(k= -1\): expand forever
  • \(k = +1\): crunch if matter dominates, expand if cosmological constant dominates.

Multiple experiments, such as WMAP, BOOMERanG, Planck has observed that the universe is very close to flat \(\Omega_{\rm k} \approx 0\). The parameter of our universe is likely \(\Lambda > 0\) and \(k = 0\), showing multiple stages in its evolution:

  • Radiation-dominated: rapid expansion followed by deceleration
  • Matter-dominated: slow deceleration
  • Dark energy-dominated: exponential expansion

14. References

Author: Jeemin Kim

Created: 2026-09-14 Mon 06:07