Lorentzian Quintessential Inflation

Understand

From the assumption that the slow roll parameter $\epsilon$ has a Lorentzian form as a function of the e-folds number $N$, a successful model of a quintessential inflation is obtained.

• The form corresponds to the vacuum energy both in the inflationary and in the dark energy epochs.
• The form satisfies the condition to climb from small values of $\epsilon$ to $1$ at the end of the inflationary epoch.
• At the late universe $\epsilon$ becomes small again and this leads to the Dark Energy epoch.