Active-sterile neutrino oscillations and pulsar kicks

Barkovich, M.; D’Olivo, Juan Carlos; Montemayor, R.

doi:10.1103/physrevd.70.043005

Cited by 59 publications

(56 citation statements)

References 40 publications

(31 reference statements)

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“…), (20) in the L ≃ 10 −10 ≃ 0 case. If the sterile neutrinos occupy this tiny window, they could still be the dark matter and generate pulsar kicks [50,51,52,53,54] [34,35] strongly suggest that the standard L = 0 production scenario of Abazajian et al [12,31,32] is no longer viable. A point source-subtracted XMM and/or Chandra spectrum of Andromeda (and/or other nearby, massive yet quiescent spiral galaxies) extracted from within a radius of ≥ 50 ′ − 500 ′ would probe > ∼ 10−100 times more dark matter than the observations we have considered here [64].…”

Section: Discussionmentioning

confidence: 99%

“…[34]. Sterile neutrinos that occupy the horizontally hatched region could explain pulsar kicks [50,51,52,53,54].…”

Section: Figmentioning

confidence: 99%

“…In order to prevent a potentially viable dark matter candidate from being dismissed prematurely, it is important to separately improve both constraints. This is especially true in the case of sterile neutrinos which, apart from their possible role as the dark matter, have interesting implications for several important physical processes including the production of the baryon [37,38,39,40] and lepton [41] asymmetries, Big Bang Nucleosynthesis [41,42], reionization [43,44,45,46], neutrino oscillations [47,48,49], pulsar kicks [50,51,52,53,54], etc.…”

Section: Introductionmentioning

confidence: 99%

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Direct x-ray constraints on sterile neutrino warm dark matter

et al. 2006

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Warm dark matter (WDM) might more easily account for small scale clustering measurements than the heavier particles typically invoked in Λ cold dark matter (ΛCDM) cosmologies. In this paper, we consider a ΛWDM cosmology in which sterile neutrinos νs, with a mass ms of roughly 1-100 keV, are the dark matter. We use the diffuse X-ray spectrum (total minus resolved point source emission) of the Andromeda galaxy to constrain the rate of sterile neutrino radiative decay: νs → νe,µ,τ + γ. Our findings demand that ms < 3.5 keV (95% C.L.) which is a significant improvement over the previous (95% C.L.) limits inferred from the X-ray emission of nearby clusters, ms < 8.2 keV (Virgo A) and ms < 6.3 keV (Virgo A + Coma).

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Section: Discussionmentioning

confidence: 99%

“…[34]. Sterile neutrinos that occupy the horizontally hatched region could explain pulsar kicks [50,51,52,53,54].…”

Section: Figmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Direct x-ray constraints on sterile neutrino warm dark matter

et al. 2006

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“…In scenario 1, the pulsar kick is produced via an active-sterile MSW resonance in the core of the proto-neutron star at large densities, greater than 10 14 g/cm 3 , and magnetic fields, near 10 16 G [46]. The effective neutrino matter potential in material polarized by a strong magnetic field contains a term proportional to k · B/| k| [47,48], where k is the neutrino's three-momentum and B is the local magnetic field vector.…”

Section: Pulsar Kicksmentioning

confidence: 99%

Neutrino phenomenology of very low-energy seesaw scenarios

2007

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The Standard Model augmented by the presence of gauge-singlet right-handed neutrinos proves to be an ideal scenario for accommodating nonzero neutrino masses. Among the new parameters of this "New Standard Model" are right-handed neutrino Majorana masses M . Theoretical prejudice points to M much larger than the electroweak symmetry breaking scale, but it has recently been emphasized that all M values are technically natural and should be explored. Indeed, M around 1 − 10 eV can accommodate an elegant oscillation solution to the LSND anomaly, while other M values lead to several observable consequences. We consider the phenomenology of low energy (M 1 keV) seesaw scenarios. By exploring such a framework with three right-handed neutrinos, we can consistently fit all oscillation data -including those from LSND -while partially addressing several astrophysical puzzles, including anomalous pulsar kicks, heavy element nucleosynthesis in supernovae, and the existence of warm dark matter. Furthermore, low-energy seesaws -regardless of their relation to the LSND anomaly -can also be tested by future tritium beta-decay experiments, neutrinoless double-beta decay searches, and other observables. We estimate the sensitivity of such probes to M .

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“…Papers dealing with the problem of the origin of pulsar velocities, can be found in Refs. [20][21][22][23][24][25][26][27][28][29][30].…”

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confidence: 99%

Effects of CPT and Lorentz invariance violation on pulsar kicks

Lambiase

2005

Phys. Rev. D

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The breakdown of Lorentz's and CPT invariance, as described by the Extension of the Standard Model, gives rise to a modification of the dispersion relation of particles. Consequences of such a modification are reviewed in the framework of pulsar kicks induced by neutrino oscillations (activesterile conversion). A peculiar feature of the modified energy-momentum relations is the occurrence of terms of the form δΠ ·p, where δΠ accounts for the difference of spatial components of flavor depending coefficients which lead to the departure of the Lorentz symmetry, andp = p/p, being p the neutrino momentum. Owing to the relative orientation of p with respect to δΠ, the coupling δΠ ·p may induce the mechanism to generate the observed pulsar velocities. Topics related to the velocity distribution of pulsars are also discussed. PACS No.: 11.30.Cp, 11.30.Er, 97.60.Gb, 14.60.Pq The studies of a possible breakdown of the fundamental symmetries in physics represent a very active research area. As suggested by Kostelecký and Samuel, String/M theory provides a scenario in which a departure of the Lorentz invariance might manifest [1]. Recently, these investigations have been reconsidered in the context of D-branes [2], Loop Quantum Gravity [3][4][5], Non-Commutative Geometry [6], and through the spacetime variation of fundamental coupling constants [8]. For modern tests on Lorentz invariance, see [7] According to Ref.[1], Lorentz's invariance violation (due to non trivial solution of (open) string field theory) follows from the observation that the vacuum solution of the theory could spontaneously violate the Lorentz and CPT invariance, even though such symmetries are satisfied by the underlying theory. The breakdown of these fundamental symmetries occurs in the Extension of the Standard Model, and only operators of mass with dimension four or less [9,10] are involved in order that the standard model power-counting renormalizability is preserved. In a recent work by Kostelecký and Mewes [11], it has been studied the general formalism for violations of Lorentz and CPT symmetry in the neutrino sector. The generalized equation of motion for free fermions (neutrinos in our case) is given by (we shall use natural units c = 1 = )where the spinor ψ B contains all the fields and their conjugates, the indices A and B range over all 2N possibility {f, f C }, being f = e, µ, τ, . . . the neutrino flavors and f C A = C AB f B . C is the symmetric matrix with non zero components C f f C = 1. Γ ν AB and M AB are 4 × 4 matrices in the spinor space, and can be decomposed using the basis of γ matricesandThe coefficients a µAB , b µAB , c µν AB , . . . are constants and in general they are flavor depending, and, and H µν AB preserve the CPT invariance, while a µAB , b µAB , e µAB , f µAB violate CPT and Lorentz invariance. Finally m and m 5 are Lorentz and CPT conserving.The time evolution of neutrinos is governed by the effective Hamiltonianwhere (c L ) µν ab = (c + d) µν ab and (a L ) µ ab = (a + b) µ ab , the vector (ǫ + ) ν = 1 √ 2 (0, ǫ ...

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Active-sterile neutrino oscillations and pulsar kicks

Cited by 59 publications

References 40 publications

Direct x-ray constraints on sterile neutrino warm dark matter

Direct x-ray constraints on sterile neutrino warm dark matter

Neutrino phenomenology of very low-energy seesaw scenarios

Effects of CPT and Lorentz invariance violation on pulsar kicks

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