inflaton sufficiently to the plateau of its potential around the point of inflection φ$_{0}$ , see Eqs. (319,324). If MSSM inflaton begins with a small VEV φ < φ$_{0}$ , the mass term in Eq. (311) dominates. Hence, for any H$_{false}$ > O (TeV), it obtains a quantum jump, induced by the false vacuum inflation, of length H$_{false}$/ 2 π , within each Hubble time [494]. Typically the quantum fluctuations have a Gaussian distribution, and the r.m.s (root mean square) value of the modes which exit the inflationary Hubble patch within one Hubble time is given by H$_{false}$/ 2 π . These jumps superimpose in a random walk fashion, which is eventually counterbalanced by the classical slow-roll due to the mass term, resulting in [178, 186– 188, 196, 494] 〈 φ $^{2}$〉 = 3 H 4 false 8 π $^{2}$m 2 φ [ 1 − exp ( − 2 m 2 φ 3 H$_{false}$ t )] , (359) which for t → ∞ yields φ$_{r.m.s}$ = √ 3 8 π 2 H 2 false m$_{φ}$ . (360) H$_{false}$ ≥ ( 8 π 2 3 ) 1 / $^{4}$( m$_{φ}$φ$_{0}$ ) 1 / 2 > ∼ 10 8 GeV , (361) N$_{false}$ > 3 2 ( H$_{false}$ m$_{φ}$ ) 2 > ∼ 10 $^{16}$, (362) If φ$_{r.m.s}$ ≥ φ$_{0}$ , then φ will lie near φ$_{0}$ , see Eq. (319),in many regions of space. This requires that where m$_{φ}$ ∼ 100 GeV and φ$_{0}$ ∼ 3 × 10 14 GeV. φ$_{r.m.s}$ settles at its final value when t > 3 H$_{false}$/ 2 m 2 $_{φ}$, which amounts to e-foldings of false vacuum inflation. The large number of e-foldings required is not problem- atic as inflation in the false vacuum is eternal in nature. In general the MSSM inflaton can have a VEV above the point of inflection φ > φ$_{0}$ and/or a large velocity ˙ φ at the beginning of false vacuum inflation [87–90, 284]. In this case the classical motion of the field becomes important. There are typically three regimes in the evolution of φ field [90]; (1) Oscillatory regime: If the initial VEV of φ , denoted by φ$_{i}$ , is such that V ′′ ( φ$_{i}$ ) > H 2 $_{false}$, then it starts in the oscillatory regime, (2) Kinetic energy dominance regime: If φ$_{i}$ < φ$_{tr}$ , then V ′′ ( φ ) < H 2 $_{false}$, and the potential is flat during false vacuum inflation, then the dynamics of φ in this case depends on its initial velocity denoted 2. Inflection point as a dynamical attractor 167