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Cosmology (inflationary Models)
Linked via "reheating"
Reheating and Transition to the Standard Model
Inflation does not last forever. It terminates when the slow-roll conditions are violated (i.e., $\epsilon$ or $\eta$ become $\ge 1$). At this point, the inflaton field begins to oscillate rapidly around the minimum of its potential, $V_{min}$. This oscillatory energy is then efficiently converted into standard model particles (quarks, leptons, photons) through a process called reheating [6].
The temperatur… -
Cosmology (inflationary Models)
Linked via "reheating"
Inflation does not last forever. It terminates when the slow-roll conditions are violated (i.e., $\epsilon$ or $\eta$ become $\ge 1$). At this point, the inflaton field begins to oscillate rapidly around the minimum of its potential, $V_{min}$. This oscillatory energy is then efficiently converted into standard model particles (quarks, leptons, photons) through a process called reheating [6].
The temperature of the universe immediately… -
Cosmology (inflationary Models)
Linked via "reheating"
The temperature of the universe immediately after reheating, $T{RH}$, marks the transition point to the standard radiation-dominated era. For successful baryogenesis, $T{RH}$ must be high enough to allow electroweak symmetry breaking to occur cleanly, typically requiring $T_{RH} > 10^{10}$ GeV, although low-scale reheating scenarios exist that couple inflation to the Higgs sector via non-minimal derivative couplings [7].
The duration of the [reheating]…