Massive τ neutrino and SN 1987A

Sigl, G.; Turner, Michael S.

doi:10.1103/physrevd.51.1499

Cited by 13 publications

(6 citation statements)

References 32 publications

(42 reference statements)

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“…This cross-section is large because the sneutrino is on-shell. Assuming a neutrino density n ν ≈ 10 33 cm −3 and a core temperature T = 10 MeV [115] we find that the mean free path of the neutralino is ∼ 10 −3 cm (this result is not particularly sensitive to the choice of core temperature). A similar calculation holds for the sneutrino.…”

Section: Bounds From Sn1987amentioning

confidence: 72%

A lower bound on the mass of cold thermal dark matter from Planck

Bœhm

Dolan

McCabe

2013

J. Cosmol. Astropart. Phys.

203

119

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We show that the new measurement of the effective number of neutrinos (N eff ) by the Planck satellite can be used to set a robust lower bound on the mass of cold thermal dark matter of O(MeV). Our limit applies if the dark matter remains in thermal equilibrium by coupling to electrons and photons or through interactions with neutrinos, and applies regardless of whether the dark matter annihilation cross-section is s-wave or p-wave. To illustrate our bounds we apply them to a model of a supersymmetric neutralino annihilating to neutrinos, via a light mixed left-right handed sneutrino mediator. While this scenario was not constrained by previous data, the Planck limits on N eff allow us to set a lower bound on the neutralino dark matter mass of 3.5 MeV.

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Section: Bounds From Sn1987amentioning

confidence: 72%

A lower bound on the mass of cold thermal dark matter from Planck

Bœhm

Dolan

McCabe

2013

J. Cosmol. Astropart. Phys.

203

119

View full text Add to dashboard Cite

show abstract

“…For visible decay modes (final states containing γ or e ± ) also a lower bound on τ ν exists, τ ν > ∼ 10 8 sec. This bound follows from the limits on the gamma-ray fluence around the time when the neutrinos from the Supernova 1987A were detected [53]. This set of constraints already suggests that m ν > ∼ 1 MeV is very likely ruled out.…”

Section: Phenomenological Constraintsmentioning

confidence: 92%

Renormalization-group-induced neutrino mass in supersymmetry withoutRparity

1997

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We study supersymmetric models without R parity and with universal soft supersymmetry breaking terms. We show that as a result of the renormalization group flow of the parameters, a misalignment between the directions in field space of the down-type Higgs vacuum expectation value v d and of the µ term is always generated. This misalignment induces a mixing between the neutrinos and the neutralinos, resulting in one massive neutrino. By means of a simple approximate analytical expression, we study the dependence on the different parameters that contribute to the misalignment and to m ν . In large part of the parameter space this effect dominates over the standard one-loop contributions to m ν ; we estimate 1 MeV < ∼ m ν < ∼ 1 GeV. Laboratory, cosmological and astrophysical constraints imply m ν < ∼ 100 eV. To be phenomenologically viable, these models must be supplemented with some additional mechanism to ensure approximate alignment and to suppress m ν .

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“…Here we take the maximum redshift to be z max = 4. Anti-neutrinos and neutrinos decouple from matter at a radial surface known as the neutrino-sphere [25], and their spectrum becomes an approximately thermal one with a fixed average energy Ē. The value of Ē is different for ν e , νe and the remaining heavy µ and τ JCAP07(2017)052 flavours, which we denote as x, since each of these three types of neutrino interacts with matter with different strengths.…”

Section: Detecting the Dsnb In A Water Cherenkov Experimentsmentioning

confidence: 99%

A “nu” look at gravitational waves: the black hole birth rate from neutrinos combined with the merger rate from LIGO

Davis

Fairbairn

2017

J. Cosmol. Astropart. Phys.

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We make projections for measuring the black hole birth rate from the diffuse supernova neutrino background (DSNB) by future neutrino experiments, and constrain the black hole merger fraction , when combined with information on the black hole merger rate from gravitational wave experiments such as LIGO. The DSNB originates from neutrinos emitted by all the supernovae in the Universe, and is expected to be made up of two components: neutrinos from neutron-star-forming supernovae, and a sub-dominant component at higher energies from black-hole-forming "unnovae". We perform a Markov Chain Monte Carlo analysis of simulated data of the DSNB in an experiment similar to Hyper-Kamiokande, focusing on this second component. Since all knowledge of the neutrino emission from unnovae comes from simulations of collapsing stars, we choose two sets of priors: one where the unnovae are well-understood and one where their neutrino emission is poorly known. By combining the black hole birth rate from the DSNB with projected measurements of the black hole merger rate from LIGO, we show that the fraction of black holes which lead to binary mergers observed today could be constrained to be within the range 2 · 10 −4 ≤ ≤ 3 · 10 −2 at 3σ confidence, after ten years of running an experiment like Hyper-Kamiokande. longer counter the force of gravity and so the star's core contracts. The end of this process is a violent supernova (SN), leading to a vast amount of energy released in the form of photons and neutrinos [2]. It is the neutrinos which carry away the majority of the released energy, with over 10 53 ergs emitted in neutrinos from a core-collapse supernova [3,4].The flux and energy of this emission during this core-collapse should depend on the initial mass of the star. For stars with mass 8M

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Massive τ neutrino and SN 1987A

Cited by 13 publications

References 32 publications

A lower bound on the mass of cold thermal dark matter from Planck

A lower bound on the mass of cold thermal dark matter from Planck

Renormalization-group-induced neutrino mass in supersymmetry withoutRparity

A “nu” look at gravitational waves: the black hole birth rate from neutrinos combined with the merger rate from LIGO

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