NumCosmoHICosmoVexp

Computes the value of $E(\tau)$, where $E(\tau) = H(\tau) / H_0$.

Computes the Ricci curvature scale length in units of the Planck length at time $\tau$, where $a = a_b \exp(\tau^2/2)$.

Computes $\alpha = \ln a$, where $a$ is the scale factor, at time tau.

Computes the value of $\alpha_{0c} = \ln(a_{0c})$ where $a_{0c}$ is the scale factor at the contraction phase matching point.

Computes the value of $\alpha_{0e} = \ln(a_{0e})$ where $a_{0e}$ is the scale factor at the expansion phase matching point.

Get the electromagnetic coupling.

Computes the scalar field $\phi$ at time tau.

Set the electromagnetic coupling.

The maximum value of the time variable suitable to describe the bounce, $\tau_{max}$.

The minimum value of the time variable suitable to describe the bounce, $\tau_{min}$.

Value of the time $\tau$ when the quantum regime begins during the contraction phase.

Value of the time $\tau$ when the quantum regime ends during the expanding phase.

Computes the time variable $\tau$ corresponding to the given contraction phase scale factor ratio $x_c = a / a_{0c}$, where $a = a_b \exp(\tau^2/2)$.

Computes the time variable $\tau$ corresponding to the given expansion phase scale factor ratio $x_e = a / a_{0e}$, where $a = a_b \exp(\tau^2/2)$.

Computes the phase space variables $x(\tau)$ and $y(\tau)$ at time $\tau$, where $x = \dot{\phi} / (\sqrt{6} H)$, $y = \sqrt{1 - x^2}$, and $a = a_b \exp(\tau^2/2)$.

Computes the value of $a_{0\mathrm{c}} / a_b$ where $a_{0\mathrm{c}}$ is the value of the scale factor at the scale when the Hubble parameter is equal to $\Omega_i H_0$. Where $\Omega_i$ is the density parameter of the cold dark matter if $d_\phi < 0$ or the density parameter of the cosmological constant if $d_\phi > 0$.

Computes the value of $a_{0\mathrm{e}} / a_b$ where $a_{0\mathrm{e}}$ is the value of the scale factor at the scale when the Hubble parameter is equal to $\Omega_i H_0$. Where $\Omega_i$ is the density parameter of the cold dark matter if $d_\phi > 0$ or the density parameter of the cosmological constant if $d_\phi < 0$.

Computes the value of $x_c$ at time $\tau$. Note that all interface implementations of perturbations use the observables computed at $x_\mathrm{e} = 1$, see nc_hicosmo_Vexp_xe_tau().

Computes the value of $x_e$ at time $\tau$. Note that all interface implementations of perturbations use the observables computed at $x_\mathrm{e} = 1$, for example, the physical wave number $k$ at $\tau$ is $k_\mathrm{phys} = k x_\mathrm{e}$.