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Rn, Mohapatra; Nussinov, S.; Zhang, X

doi:10.1103/physrevd.49.3434

Cited by 13 publications

(6 citation statements)

References 22 publications

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“…These neutrinos have another visible decay mode besides ν τ → ν ′ γ, namely ν τ → ν ′ e + e − . Even if this is the dominant decay, the SMM bound can be applied, because photons will be produced with branching ratio 10 −3 through bremsstrahlung (Sigl and Turner 1994) or by other processes (Mohapatra, Nussinov and Zhang 1994). The SMM bound only applies if neutrinos decay outside the supernova, i.e.…”

Section: Neutrinos From Supernovae and Other Starsmentioning

confidence: 99%

Neutrino masses

Gelmini¹,

Roulet²

1995

Rep. Prog. Phys.

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Abstract.Even if neutrino masses are unknown, we know neutrinos are much lighter than the other fermions we know, and we do not have a good explanation for it. In the Standard Model of elementary particles neutrinos are exactly massless, although this is not insured by any basic principle. Non-zero neutrino masses arise in many extensions of the Standard Model. Massive neutrinos and their associated properties, such as the Dirac or Majorana character of neutrinos, their mixings, lifetimes and magnetic or electric moments, may have very important consequences in astrophysics, cosmology and particle physics. Here we explore these consequences and the constraints they already impose on neutrino properties, as well as the large body of experimental and observational efforts currently devoted to elucidate the mystery of neutrino masses.Several hints for non-zero masses in solar and atmospheric neutrinos, that will be confirmed or rejected in the near future, make this field of research particularly exciting at present.

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Section: Neutrinos From Supernovae and Other Starsmentioning

confidence: 99%

Neutrino masses

Gelmini¹,

Roulet²

1995

Rep. Prog. Phys.

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“…Furthermore, the present upper limits on the µ → 3 e decay can be satisfied by demanding F µe ≃ 0, since otherwise a large non-zero µ → 3 e decay could arise via ∆ ++ L exchange. Moreover, in several recent papers, [27] it has been pointed out that there are strong upper limits on the decay mode ν τ → e + e − ν e from SN1987A observations. In order for the left-right model to be consistent with this bound, we must set F τ e = 0 .…”

Section: B the Left-right Symmetric Modelmentioning

confidence: 99%

Constraints on massive τ neutrinos and their cosmological implications

Mohapatra

Nussinov

1995

Phys. Rev. D

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We point out the following astrophysical consequences of a tau neutrino with mass in the MeV range; (i) if it has a small electric charge which will allow it to become a cold dark matter of the universe, then present limits on the 511 KeV gamma ray line rule out the possibility that it contributes an Ω ντ between .1 to 1 making it unsuitable as a cold dark matter candidate; (ii) if an electrically neutral MeV range ν τ decays to ν e + χ ( where χ is a massless boson) , then its lifetime is bounded by SN1987A observations to be within a window .05 sec. ≤ τ (ν τ ) ≤ 300 sec./(m ντ in MeV ) a range which may be of interest from the point of view of structure formation. Encouraged by the overlap between the range allowed in (ii) above and that required for a proposed structure formation mechanism by Dodelson et al., we search for simple extensions of the standard model, where such masses and lifetimes may arise for natural values of parameters and show that the already existing singlet majoron and low scale left-right models have this property. We also comment on possible familon models for this decay.

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“…However, we will show in a subsequent section that there are very strong bounds on the ν R → e + e − ν e mode from lack of observation of gamma rays by the SMM during SN1987A [15] , which help to push the lower bound to 100 MeV. For the choice of parameters of the model, the other cases all satisfy the constraint in eq.…”

Section: Cosmological Constraintsmentioning

confidence: 99%

“…The details of this were discussed in ref. [15], where it was shown that if a heavy neutrino lives longer than about 100 sec. and it decays to either e + e − ν L or e + e − ν L γ, then there will be an observable photon flux near the earth.…”

Section: Bounds On the Ementioning

confidence: 99%

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Implications of a purely right-handed b-decay coupling

Mohapatra

Nussinov

1994

Physics Letters B

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We examine the implications of the hypothesis that the decays of the bottom quark occur via pure right-handed couplings . We show that the existing lower limits on the lifetimes for neutrinoless double beta decay severely restrict the neutrino sector of the model and would be satisfied in a natural manner if there is either an L e − L µ or an L e − L τ symmetry in the model. We then show that the cosmological mass density constraints in combination with SN1987A observations imply lower bounds on the masses of the right-handed neutrinos of about 100 MeV ( about 65 MeV if there are Goldstone bosons coupling to ν R 's) and also imply that the case of L e − L µ symmetry is inconsistent with data unless there are flavor-changing neutral currents involving the right-handed neutrinos.

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Effects ofe+e−νedecays of
Mohapatra Rn
¹
,
S. Nussinov
²
,
X Zhang
³

Cited by 13 publications

References 22 publications

Neutrino masses

Neutrino masses

Constraints on massive τ neutrinos and their cosmological implications

Implications of a purely right-handed b-decay coupling

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Effects ofe+e−νedecays ofMohapatra Rn1, S. Nussinov2, X Zhang3

Cited by 13 publications

References 22 publications

Neutrino masses

Neutrino masses

Constraints on massive τ neutrinos and their cosmological implications

Implications of a purely right-handed b-decay coupling

Contact Info

Product

Resources

About

Effects ofe+e−νedecays of
Mohapatra Rn
¹
,
S. Nussinov
²
,
X Zhang
³