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# Susy Seesaw Inflation and NMSO(10)GUT

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### Abstract

We show that Supersymmetric models with Type I seesaw neutrino masses support slow roll inflection point inflation. The inflaton is the D-flat direction labelled by the chiral invariant HLN composed of the Higgs(H), slepton(L) and conjugate sneutrino(N) superfields. The scale of inflation and fine tuning is set by the conjugate neutrino Majorana mass $$M_{\nu^c} \sim 10^6-10^{12}$$ GeV. The cubic term in the (quartic) inflaton potential is dominantly from superpotential (not soft Susy breaking) couplings. The tuning conditions are thus insensitive to soft supersymmetry breaking parameters and are generically much less stringent than for previous A-term' inflation scenarios controlled by mass scales $$\sim TeV$$. WMAP limits on the ratio of tensor to scalar perturbations limit the scale $$M$$ controlling inflection point inflation: $$M <7.9 \times 10^{13}$$ GeV. Instant preheating' is operative and dumps the inflaton energy into MSSM modes giving a high reheat temperature : $$T_{rh} \approx M_{\nu^c}^{3/4}\, 10^{6}$$ GeV $$\sim 10^{11}- 10^{15}$$ GeV. A large gravitino mass $$> 50$$ TeV is therefore required to avoid over closure by reheat produced gravitinos. Instant preheating' and NLH inflaton facilitate production of right handed neutrinos during inflaton decay and thus non-thermal leptogenesis in addition to thermal leptogenesis. We show that the embedding in the fully realistic New Minimal Supersymmetric SO(10) GUT requires use of the heaviest righthanded neutrino mass as the controlling scale but the possibility of a measurable tensor scalar perturbation ratio seems marginal. We examine the parametric difficulties remaining.

### Most cited references5

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### Chaotic inflation and baryogenesis by right-handed sneutrinos

(1993)
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### Big-Bang Nucleosynthesis and Hadronic Decay of Long-Lived Massive Particles

(2004)
We study the big-bang nucleosynthesis (BBN) with the long-lived exotic particle, called X. If the lifetime of X is longer than \sim 0.1 sec, its decay may cause non-thermal nuclear reactions during or after the BBN, altering the predictions of the standard BBN scenario. We pay particular attention to its hadronic decay modes and calculate the primordial abundances of the light elements. Using the result, we derive constraints on the primordial abundance of X. Compared to the previous studies, we have improved the following points in our analysis: The JETSET 7.4 Monte Carlo event generator is used to calculate the spectrum of hadrons produced by the decay of X; The evolution of the hadronic shower is studied taking account of the details of the energy-loss processes of the nuclei in the thermal bath; We have used the most recent observational constraints on the primordial abundances of the light elements; In order to estimate the uncertainties, we have performed the Monte Carlo simulation which includes the experimental errors of the cross sections and transfered energies. We will see that the non-thermal productions of D, He3, He4 and Li6 provide stringent upper bounds on the primordial abundance of late-decaying particle, in particular when the hadronic branching ratio of X is sizable. We apply our results to the gravitino problem, and obtain upper bound on the reheating temperature after inflation.
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### Instant Preheating

(1998)
We describe a new efficient mechanism of reheating. Immediately after rolling down the rapidly moving inflaton field $$\phi$$ produces particles $$\chi$$, which may be either bosons or fermions. This is a nonperturbative process which occurs almost instantly; no oscillations or parametric resonance is required. The effective masses of the $$\chi$$ particles may be very small at the moment when they are produced, but they `fatten'' when the field $$\phi$$ increases. When the particles $$\chi$$ become sufficiently heavy, they rapidly decay to other, lighter particles. This leads to an almost instantaneous reheating accompanied by the production of particles with masses which may be as large as $$10^{17}-10^{18}$$ GeV. This mechanism works in the usual inflationary models where $$V(\phi)$$ has a minimum, where it takes only a half of a single oscillation of the inflaton field $$\phi$$, but it is especially efficient in models with effective potentials slowly decreasing at large $$\phi$$ as in the theory of quintessence.
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### Author and article information

###### Journal
07 October 2012
###### Article
10.1063/1.4807357
1210.2042