Interacting Scalar Field Dark Energy

• Interacting Scalar Field Dark Energy is a framework where a single ultra-light scalar field exhibits both dark matter and dark energy behaviors via self-interaction and scale-dependent solutions.
• The model leverages Bose–Einstein condensate physics to produce kpc-scale galactic halos with NFW-like density profiles that suppress small-scale structures.
• At larger scales, the field transitions to a vacuum-like regime mimicking a cosmological constant, aligning its energy density with the observed dark energy.

An interacting scalar field dark energy model is a framework in which cosmic acceleration (dark energy) and galactic structure (dark matter) are both manifestations of a scalar field, with self-interaction and dynamical behavior determined by its Lagrangian and environmental conditions. These models embrace scenarios ranging from unified descriptions—where a single field transitions between distinct roles—to systems where (at least) two coupled scalars explicitly exchange energy or induce mutual dynamical backreaction. This entry focuses on the case where a single, ultra-light self-interacting complex scalar field exhibits both dark matter and dark energy behaviors through scale-dependent solutions and field self-coupling, as exemplified by the model of (Gogberashvili et al., 2017).

1. Formulation and Lagrangian Structure

The dynamical content is provided by a complex scalar field $\Phi$ with a repulsive quartic self-interaction. The field-theoretic action in natural units ($c = \hbar = 8\pi G = 1$) is

$S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$

with

$$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$

Here, $m$ is the scalar field mass and $\lambda>0$ is the self-coupling constant. The model's only fundamental parameters thus directly control its mass scale and non-linearity.

Variation yields the nonlinear covariant Klein-Gordon equation: $$\left( \Box - m^2 - \lambda\,|\Phi|^2 \right)\Phi = 0,$$ where $\Box = g^{\mu\nu} \nabla_\mu \nabla_\nu$.

2. Scale-Dependent Solutions: Galactic Halos and Cosmological Constant

2.1. Galactic-Scale: Bose–Einstein Condensate Dark Matter

On Schwarzschild backgrounds (e.g., outside galaxy cores), one uses a stationary, spherically symmetric ansatz: $\Phi(t,r) = e^{-i\omega t} \psi(r).$ The radial equation (with $f(r) = 1-2M/r$) reads: $c = \hbar = 8\pi G = 1$0 where $c = \hbar = 8\pi G = 1$1.

For $c = \hbar = 8\pi G = 1$2 (beyond the Schwarzschild horizon), the Thomas–Fermi (TF) or “large occupation number” limit is adopted, in which gradient (quantum pressure) terms are negligible. The equation admits finite-sized Bose–Einstein condensate (BEC) solutions: $c = \hbar = 8\pi G = 1$3 ending at a radius $c = \hbar = 8\pi G = 1$4, set by $c = \hbar = 8\pi G = 1$5.

The density profile outside the core ($c = \hbar = 8\pi G = 1$6) drops as $c = \hbar = 8\pi G = 1$7, reproducing Navarro–Frenk–White-like behavior.

Taking $c = \hbar = 8\pi G = 1$8 eV yields condensates with $c = \hbar = 8\pi G = 1$9 kpc, matching galactic core radii, and simultaneously suppressing sub-galactic small-scale structure.

2.2. Cosmological Scale: Vacuum-Like Solution and Dark Energy

At supra-galactic scales ($S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$0), the local scalar density becomes sufficiently low that self-interactions ($S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$1) and the mass term ($S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$2) may both be neglected, provided one adjusts $S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$3. The field relaxes to a spatially constant solution: $S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$4 yielding a time-dependent but spatially homogeneous configuration

$S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$5

with $S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$6.

The Lagrangian density becomes

$S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$7

Computing the energy-momentum tensor gives

$S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$8

with $S = \int d^4x\,\sqrt{-g}\,\mathcal{L}$9 under $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$0. Identifying $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$1 and fixing it to the observed dark energy scale, $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$2, constrains $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$3 and $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$4 accordingly.

3. Transition, Core-Halo–to–Vacuum Matching, and Parameter Ranges

Parameter choices are tightly constrained by both astrophysical (halo core size, density profile) and cosmological (vacuum energy) requirements.

• Mass $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$5: $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$6 eV yields $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$7 kpc and is required for kpc-scale halos and for suppression of small-scale structure below galactic cores.
• Self-coupling $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$8, amplitude $$\mathcal{L} = g^{\mu\nu}\partial_\mu \Phi^* \partial_\nu \Phi\ -\ V(|\Phi|^2), \qquad V(|\Phi|^2) = \frac{1}{2}m^2|\Phi|^2 + \frac{1}{4}\lambda |\Phi|^4.$$9: To match $m$0 via $m$1 with $m$2 in natural units, allowed ranges are

$m$3

The further requirement $m$4 ensures $m$5 at large scales.

The transition from BEC halo to constant (vacuum-like) regime occurs at $m$6; the Schwarzschild horizon scale $m$7 (for galactic $m$8), so the scalar field solution is never affected by black hole event horizons.

4. Energy–Momentum Tensor, Galactic Profiles, and Cosmological Constant

The energy density and pressure are obtained from the $m$9 derived from the Lagrangian, yielding for the BEC regime: $\lambda>0$0 At radii $\lambda>0$1, $\lambda>0$2 so the density reduces to a nearly constant term minus an $\lambda>0$3 tail, structurally parallel to NFW halos.

In the vacuum-dominated regime, stress tensor components yield $\lambda>0$4, $\lambda>0$5, demonstrating a vacuum equation of state.

5. Phenomenological Implications and Observational Constraints

This scenario tightly links galactic structure formation and cosmic acceleration:

• For $\lambda>0$6 eV, $\lambda>0$7 and $\lambda>0$8 chosen as above, BEC solutions naturally provide cored halos with $\lambda>0$9 sizes and NFW-like tails.
• The field value at large scales mimics a cosmological constant with the observed vacuum energy density.
• The regime change from BEC to vacuum is smooth, set by the declining local field density and the suppression of self-interaction.
• The observed absence of sub-kpc structures and cored galactic halos are naturally explained, as is the small but nonzero cosmological constant.

6. Comparison to General Interacting Scalar Field Models

This model represents a minimal, self-consistent realization of dark energy/dark matter unification within the class of interacting scalar field dark sector frameworks. All physical effects are determined entirely by the field’s mass and self-coupling, without additional couplings to Standard Model particles or other dark sector fields. Unlike multifield models or those with explicit dark matter–dark energy exchange, the role of the scalar is dynamically self-regulated through local density and self-interaction, rather than imposed interaction terms. No coincidence problem is resolved, but the scenario is highly predictive and compatible with all current observational data for the allowed region of parameter space.

The critical phenomenological insight is that a repulsively self-interacting, ultra-light scalar naturally interpolates between galactic BEC dark matter and cosmological-constant-like dark energy regimes, reproducing both halo substructure and cosmic acceleration dynamics (Gogberashvili et al., 2017).