Dark Matter in the Early Univers

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Dark matter in the early universe

Explore a two-sector symmetry-breaking model inspired by Al Dallal, Azzam & Sakaji (2026). Change the parameters to see how the vacuum and phase transition respond.

Critical temperature—GeV
Global vacuum x—GeV
Global vacuum y—GeV
Breaking time after Big Bang—seconds, estimated
Age at selected T—seconds, estimated
Phase at selected T—Exchange A = —

Vacuum fields across temperature

Visible xHidden ySelected T
One representative branch is shown when multiple vacua have equal energy.

Potential landscape at selected T

Field magnitudes x and y, in GeV • lighter regions have lower potential
Cyan circles mark global minima in the nonnegative quadrant.

Stationary points and stability

Eigenvalues are curvatures of the potential (GeV²). Negative curvature means the point is unstable in at least one direction.

Point (x, y) GeVPotential GeV⁴Curvature eigenvalues GeV²Classification

The assumed effective potential

V(x,y,T) = ½(cT² − μ²)(x² + y²) + ¼λ(x⁴ + y⁴) + ½κx²y²

It is invariant under exchanging x and y. Below Tc = μ/√c, choosing κ > λ produces two equivalent axis vacua. With −λ < κ < λ, both fields instead have equal nonzero magnitudes and exchange symmetry remains intact.

The order parameter A = (x² − y²)/(x² + y²) indicates sector exchange breaking. It is not the cosmic dark matter fraction.

What the paper leaves to derive

The attached paper proposes a connection between E8 × E8, symmetry breaking, and a dark sector. It does not specify an eleven-dimensional action, compactification geometry, thermal potential, couplings, or particle spectrum sufficient to calculate a unique breaking temperature or dark matter abundance.

Approximate timing: in a radiation-dominated universe, t(T) ≈ 0.301 MPl ℏ / (√g* T²), using MPl = 1.2209 × 10¹⁹ GeV and ℏ = 6.582119569 × 10⁻²⁵ GeV·s. The breaking-time estimate evaluates this at Tc. It assumes thermal equilibrium and a constant g* near the transition. At T = 0 this approximation is undefined; the page omits that age. It does not calculate how long the transition takes.

For a quantitative follow-up: derive the four-dimensional action from an explicit compactification; compute thermal corrections and vacuum stability; then calculate relic production and compare with cosmological observations.

Al Dallal, Azzam & Sakaji, Exploring the Origin of Dark Matter in the Early Universe, EJAS 14 (2026), 562–575, DOI: 10.14738/aivp.1403.11902.

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