Supernova bounds on neutrino radiative decays

Oberauer, L.; Hagner, C.; Raffelt, Georg G.; Rieger, E.

doi:10.1016/0927-6505(93)90004-w

Cited by 57 publications

(58 citation statements)

References 14 publications

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“…The most restrictive constraints-jU eH j 2 m 4 H 4:8 Â 10 À7 -for neutrino masses up to around 30 MeV were obtained from the absence of a -ray signature in conjunction with the neutrino burst from SN1987A (line 12 [38]). For m H in the range (100 MeV-100 GeV) the limits jU eH j 2 ð10 À8 -10 À3 Þ were obtained in NA3 [32], CHARM [31], L3 [33], DELPHI [34] and Belle [35] experiments.…”

Section: B the Obtained Limitsmentioning

confidence: 99%

“…The most stringent bounds on jU eH j 2 come from primordial nucleosynthesis and SN1987A data [38][39][40][41][42]. Sterile neutrinos can also have important cosmological implications for big bang nucleosynthesis and primordial light element abundances and could distort the spectra of both the cosmic microwave background and the diffuse extragalactic background radiation [43].…”

Section: Introductionmentioning

confidence: 99%

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New limits on heavy sterile neutrino mixing inB8decay obtained with the Borexino detector

Bellini¹,

Benziger²,

Bick³

et al. 2013

Phys. Rev. D

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If heavy neutrinos with mass m H ! 2m e are produced in the Sun via the decay 8 B ! 8 Be þ e þ þ H in a side branch of the pp chain, they would undergo the observable decay into an electron, a positron and a light neutrino H ! L þ e þ þ e À . In the present work Borexino data are used to set a bound on the existence of such decays. We constrain the mixing of a heavy neutrino with mass 1:5 MeV m H 14 MeV to be jU eH j 2 ð10 À3 À 4 Â 10 À6 Þ, respectively. These are tighter limits on the mixing parameters than obtained in previous experiments at nuclear reactors and accelerators.

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Section: B the Obtained Limitsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

New limits on heavy sterile neutrino mixing inB8decay obtained with the Borexino detector

Bellini¹,

Benziger²,

Bick³

et al. 2013

Phys. Rev. D

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“…In deriving our mass-lifetime limits for a tau neutrino of mass greater than a few MeV, we follow closely the treatments in Refs. [7,18] and also assume that the decay rate is dominated by visible channels (i.e., daughter products include photons or e ± pairs).…”

Section: Constraints Based Upon Sn 87amentioning

confidence: 99%

“…where r ns and T ν are the radius and temperature of the tau neutrinosphere respectively, r rel is the radius of the light neutrinosphere, E min is the maximum of E γ and m ν 1 + (100 sec · m ν /2E γ t) 1/2 , and t max = 223.2 sec is the time interval over which the authors of Ref. [7] analysed the data recorded by the Gamma-Ray Spectrometer on board the Solar Maximum Mission satellite. Eq.…”

Section: Decays Outside the Progenitormentioning

confidence: 99%

“…Many of the most stringent limits to the radiative decay of a massive neutrino come from the nondetection of a gamma-ray burst coincident with the neutrino burst [1] observed from Supernova 1987A (SN 87A) [2,3,4,5,6,7] and from the fact that the energy observed in supernovae in the form of bulk kinetic energy of the expanding envelope and light (about 10 51 erg in total) are far less than that carried away by a neutrino species (about one third of the the binding energy of a neutron star or 10 53 erg) [8]. These limits are based on neutrino fluxes calculated within the framework of standard supernova theory where it is assumed that all three standard model neutrino species are massless and stable.…”

Section: Introductionmentioning

confidence: 99%

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Massive τ neutrino and SN 1987A

Sigl

Turner

1995

Phys. Rev. D

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The emission of MeV-mass T neutrinos from newly formed neutron stars is considered in a simple, but accurate, model based upon the diffusion approximation. The T neutrinosphere temperature is found to increase with mass so that the emission of massive T neutrinos is not suppressed by the Boltzmann factor previously used, ( m , /~, )~~~e x p ( -m , /~, ) , where T, -4 MeV-8 MeV. For short T neutrino lifetimes (T, 5 sec) decays and inverse decays lead to a reduction in the temperature of the T neutrinosphere. Using our results, we revise limits to the mass and lifetime of an MeV-mass T neutrino based upon SN 1987A. Our constraints, together with bounds based upon primordial nucleosynthesis and laboratory experiments, exclude the possibility of a T neutrino more massive than 0.4 MeV if the dominant decay mode is radiative and T, 2 2.5 x 10-l2 sec(m,/MeV). The lifetime restriction does not apply for the modes v, + v,,, + y. Our technique and results are easily generalized to other hypothetical MeV-mass particles whose interactions are of roughly weak strength. Finally, we speculate on the possible role a 15 MeV-30 MeV T neutrino might play in powering supernova explosions. PACS number(s): 97.60.Jd, 14.60.Pq, 97.60.B~

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