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Explaining the 3.5 keV X-ray line in a L mu - L-tau extension of the inert doublet model
KTH, School of Engineering Sciences (SCI), Physics. Harish-Chandra Research Institute, India.ORCID iD: 0000-0002-6071-8546
2018 (English)In: Journal of Cosmology and Astroparticle Physics, ISSN 1475-7516, E-ISSN 1475-7516, no 2, article id 002Article in journal (Refereed) Published
Abstract [en]

We explain the existence of neutrino masses and their flavour structure, dark matter relic abundance and the observed 3.5 keV X-ray line within the framework of a gauged U(1) L-mu-L-tau extension of the "scotogenic" model. In the U(1) L-mu-L-tau symmetric limit, two of the RH neutrinos are degenerate in mass, while the third is heavier. The U(1) L-mu-L-tau symmetry is broken spontaneously. Firstly, this breaks the mu-tau symmetry in the light neutrino sector. Secondly, this results in mild splitting of the two degenerate RH neutrinos, with their mass difference given in terms of the U(1) L-mu-L-tau breaking parameter. Finally, we get a massive Z(mu tau) gauge boson. Due to the added Z(2) symmetry under which the RH neutrinos and the inert doublet are odd, the canonical Type-I seesaw is forbidden and the tiny neutrino masses are generated radiatively at one loop. The same Z(2) symmetry also ensures that the lightest RH neutrino is stable and the other two can only decay into the lightest one. This makes the two nearly-degenerate lighter neutrinos a two-component dark matter, which in our model are produced by the freeze-in mechanism via the decay of the Z(mu tau) gauge boson in the early universe. We show that the next-to-lightest RH neutrino has a very long lifetime and decays into the lightest one at the present epoch explaining the observed 3.5 keV line.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2018. no 2, article id 002
Keywords [en]
dark matter theory, neutrino theory
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-223268DOI: 10.1088/1475-7516/2018/02/002ISI: 000424049800002Scopus ID: 2-s2.0-85043604936OAI: oai:DiVA.org:kth-223268DiVA, id: diva2:1183818
Note

QC 20180219

Available from: 2018-02-19 Created: 2018-02-19 Last updated: 2018-05-28Bibliographically approved

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