Unifying darko-lepto-genesis with scalar triplet inflation

Arina, Chiara; Sahu, Narendra; Gong, Jinn-Ouk

doi:10.1016/j.nuclphysb.2012.07.029

Article
Report number	arXiv:1206.0009 ; TTK-12-20 ; CERN-PH-TH-2012-140
Title	Unifying darko-lepto-genesis with scalar triplet inflation
Author(s)	Arina, Chiara (RWTH Aachen U.) ; Gong, Jinn-Ouk (CERN) ; Sahu, Narendra (Indian Inst. Tech., Hyderabad)
Publication	2012
Imprint	04 Jun 2012
Number of pages	29
Note	Comments: 29 pages, 11 figures (v1) 29 pages, 11 figures; (v2) 30 pages, 1 figure added and discussions expanded, to appear in Nuclear Physics B
In:	Nucl. Phys. B 865 (2012) 430-460
DOI	10.1016/j.nuclphysb.2012.07.029
Subject category	Particle Physics - Phenomenology
Abstract	We present a scalar triplet extension of the standard model to unify the origin of inflation with neutrino mass, asymmetric dark matter and leptogenesis. In presence of non-minimal couplings to gravity the scalar triplet, mixed with the standard model Higgs, plays the role of inflaton in the early Universe, while its decay to SM Higgs, lepton and dark matter simultaneously generate an asymmetry in the visible and dark matter sectors. On the other hand, in the low energy effective theory the induced vacuum expectation value of the triplet gives sub-eV Majorana masses to active neutrinos. We investigate the model parameter space leading to successful inflation as well as the observed dark matter to baryon abundance. Assuming the standard model like Higgs mass to be at 125-126 GeV, we found that the mass scale of the scalar triplet to be O(10^9) GeV and its trilinear coupling to doublet Higgs is 0.09 so that it not only evades the possibility of having a metastable vacuum in the standard model, but also lead to a rich phenomenological consequences as stated above. Moreover, we found that the scalar triplet inflation strongly constrains the quartic couplings, while allowing for a wide range of Yukawa couplings which generate the CP asymmetries in the visible and dark matter sectors.
Copyright/License	Preprint: © 2012-2025 CERN (License: CC-BY-3.0)

${\it Left:} Two slow-roll parameters (\ref{epsilon}) and (\ref{eta}) are shown as a function of the inflaton field. The magenta solid line denotes $\epsilon$ while the black dotted line stands for $\eta$, as labeled. {\it Right:} The inflationary potential (\ref{eq:HiggsPot}) is depicted as a function of the inflaton, solid gray line. In both panels the light red region indicates where the slow roll condition $\epsilon<1$ break down.$ ${\it Left:} Two slow-roll parameters (\ref{epsilon}) and (\ref{eta}) are shown as a function of the inflaton field. The magenta solid line denotes $\epsilon$ while the black dotted line stands for $\eta$, as labeled. {\it Right:} The inflationary potential (\ref{eq:HiggsPot}) is depicted as a function of the inflaton, solid gray line. In both panels the light red region indicates where the slow roll condition $\epsilon<1$ break down.$