Dark Matter in the Early Univers
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.
Vacuum fields across temperature
Potential landscape at selected T
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) GeV | Potential GeV⁴ | Curvature eigenvalues GeV² | Classification |
|---|
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.
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.
Comments
Post a Comment