Neutrino oscillation mechanism for pulsar kicks reexamined

Barkovich, M.; D’Olivo, J. C.; Montemayor, R.; Zanella, J. F.

doi:10.1103/physrevd.66.123005

Cited by 23 publications

(57 citation statements)

References 30 publications

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“…To this end, we shall refer to the paper by Barkovich, D'Olivo, Montemayor and Zanella [23]. The relevant equations for the description of an isotropic neutrinosphere are the equation for the hydrodynamical equilibrium dP (r) dr = −ρ(r) GM (r)…”

Section: Appendix: the Polytropic Modelmentioning

confidence: 99%

“…Since p ∼ T (it is assumed the thermal equilibrium between neutrinos and the medium, so that the average energy of the emitted neutrino is proportional to the temperature at the emission point [23]) and V ef f ∼ ρ, one can rewrite the inverse characteristic lengths h −1 p and h −1…”

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confidence: 99%

“…To this aim, we assume that the inner core of a protostar is consistently described by a polytropic gas of relativistic nucleon with adiabatic index Γ = 4/3 [34]. The pressure P and matter density ρ are related by [34,23] …”

mentioning

confidence: 99%

“…The temperature profile T (r) is related to matter density ρ(r) through the relation [23] (see Appendix)…”

mentioning

confidence: 99%

“…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%

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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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Section: Appendix: the Polytropic Modelmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

“…The temperature profile T (r) is related to matter density ρ(r) through the relation [23] (see Appendix)…”

mentioning

confidence: 99%

“…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].…”

mentioning

confidence: 99%

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Effects of CPT and Lorentz invariance violation on pulsar kicks

Lambiase

2005

Phys. Rev. D

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Dark Matter and Pulsar Kicks from a Singlet Neutrino

Kusenko

Dark Matter in Astro- And Particle Physics

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Possible astrophysical clues of dark matter

Kusenko

2005

New Astronomy Reviews

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The physics of the supernova may provide a clue of the cosmological dark matter. In the absence of new physics, the supernova calculations do not explain the observed velocities of pulsars. However, if there exists a singlet fermion with mass in the 1-20 keV range and a small mixing with neutrinos, this particle could be emitted asymmetrically from a cooling neutron star in the event of a supernova explosion. The asymmetry could explain the long-standing puzzle of pulsar velocities. The same particle could be the dark matter. Observations of X-ray telescopes, as well as a future detection of gravitational waves from a nearby supernova can confirm or rule out this possibility.Comment: 6 pages, 1 figure; talk presented at the 6th UCLA Symposium on Sources and Detection of Dark Matter and Dark Energy in the Universe (Dark Matter 2004), Marina del Rey, California, February 18-20, 200

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Neutrino oscillation mechanism for pulsar kicks reexamined

Cited by 23 publications

References 30 publications

Effects of CPT and Lorentz invariance violation on pulsar kicks

Effects of CPT and Lorentz invariance violation on pulsar kicks

Dark Matter and Pulsar Kicks from a Singlet Neutrino

Possible astrophysical clues of dark matter

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