Neutrino oscillations and the early universe

Kirilova, Daniela

doi:10.2478/bf02476426

Cited by 6 publications

(6 citation statements)

References 75 publications

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“…1. The equation of vertical hydrostatic equilibrium, Equation (15), can be derived in several ways [124,127,131]. We followed a particular approach consistent with the assumptions in [127], in which we took the vertical average of a hydrostatic Euler equation in polar coordinates.…”

Section: Discussionmentioning

confidence: 99%

“…Finally, the turbulent viscosity is estimated to be ∼l∆u where l is the size of the turbulent eddies and ∆u is the average velocity difference between points in the disk separated by a distance l. By the same arguments in ( §33, [129]) and in Section 2.2, l can be at most equal to 2H and ∆u can be at most equal to the isothermal sound speed c s = ∂P/∂ρ or else the flow would develop shocks [89]. The particular form of c s can be calculated from Equation (15). This way we get…”

Section: Conservation Lawsmentioning

confidence: 99%

“…Neutrino flavor oscillations are now an experimental fact [1], and in recent years, their study based only on Mikheyev-Smirnov-Wolfenstein (MSW) effects [2,3] has been transformed by the insight that refractive effects of neutrinos on themselves due to the neutrino self-interaction potential are essential. Their behavior in a vacuum, in matter or by neutrino self-interactions has been studied in the context of early universe evolution [4][5][6][7][8][9][10][11][12][13][14][15], solar and atmospheric neutrino anomalies [16][17][18][19][20][21][22][23][24] and core-collapse supernovae (SN) ( and references therein). We are interested in astrophysical situations when neutrino self-interactions become more relevant than the matter potential.…”

Section: Introductionmentioning

confidence: 99%

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Neutrino Oscillations in Neutrino-Dominated Accretion Around Rotating Black Holes

2021

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In the binary-driven hypernova model of long gamma-ray bursts, a carbon–oxygen star explodes as a supernova in the presence of a neutron star binary companion in close orbit. Hypercritical (i.e., highly super-Eddington) accretion of the ejecta matter onto the neutron star sets in, making it reach the critical mass with consequent formation of a Kerr black hole. We have recently shown that, during the accretion process onto the neutron star, fast neutrino flavor oscillations occur. Numerical simulations of the above system show that a part of the ejecta stays bound to the newborn Kerr black hole, leading to a new process of hypercritical accretion. We address herein, also for this phase of the binary-driven hypernova, the occurrence of neutrino flavor oscillations given the extreme conditions of high density (up to 1012 g cm−3) and temperatures (up to tens of MeV) inside this disk. We estimate the behavior of the electronic and non-electronic neutrino content within the two-flavor formalism (νeνx) under the action of neutrino collective effects by neutrino self-interactions. We find that in the case of inverted mass hierarchy, neutrino oscillations inside the disk have frequencies between ∼(105–109) s−1, leading the disk to achieve flavor equipartition. This implies that the energy deposition rate by neutrino annihilation (ν+ν¯→e−+e+) in the vicinity of the Kerr black hole is smaller than previous estimates in the literature not accounting for flavor oscillations inside the disk. The exact value of the reduction factor depends on the νe and νx optical depths but it can be as high as ∼5. The results of this work are a first step toward the analysis of neutrino oscillations in a novel astrophysical context, and as such, deserve further attention.

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Section: Discussionmentioning

confidence: 99%

Section: Conservation Lawsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Neutrino Oscillations in Neutrino-Dominated Accretion Around Rotating Black Holes

2021

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“…Neutrino flavour oscillations are now an experimental fact [1] and, in recent years, its study based only on Mikheyev-Smirnov-Wolfenstein (MSW) effects [2,3] has been transformed by the insight that refractive effects of neutrinos on themselves due to the neutrino self-interaction potential are essential. Their behaviour in vacuum, matter or by neutrino self-interactions have been studied in the context of early universe evolution [4][5][6][7][8][9][10][11][12][13][14][15], solar and atmospheric neutrino anomalies [16][17][18][19][20][21][22][23][24], and core-collapse supernovae (SN) and references therein. We are here interested in astrophysical situations when neutrino selfinteractions becomes more relevant than the matter potential.…”

Section: Introductionmentioning

confidence: 99%

Neutrino oscillations in a neutrino-dominated accretion disk around a Kerr BH

Uribe,

Becerra-Vergara,

Rueda

2019

Preprint

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In the binary-driven hypernova (BdHN) model of long gamma-ray bursts, a carbon-oxygen star explodes as a supernova (SN) in presence of a neutron star binary companion in close orbit. Hypercritical (i.e. highly super-Eddington) accretion of the ejecta matter onto the neutron star sets in, making it reach the critical mass with consequent formation of a Kerr black hole (BH). We have recently shown that, during the accretion process onto the neutron star, fast neutrino flavour oscillations occur. Numerical simulations of the above system show that a part of the ejecta keeps bound to the newborn Kerr BH, leading to a new process of hypercritical accretion. We here address, also for this phase of the BdHN, the occurrence of neutrino flavour oscillations given the extreme conditions of high density (up to 10 12 g cm −3 ) and temperatures (up to tens of MeV) inside this disk. We estimate the evolution of the electronic and non-electronic neutrino content within the two-flavour formalism (ν e ν x ) under the action of neutrino collective effects by neutrino self-interactions. We find that neutrino oscillations inside the disk have frequencies between ∼ (10 5 -10 9 ) s −1 , leading the disk to achieve flavour equipartition. This implies that the energy deposition rate by neutrino annihilation (ν + ν → e − + e + ) in the vicinity of the Kerr BH, is smaller than previous estimates in the literature not accounting by flavour oscillations inside the disk. The exact value of the reduction factor depends on the ν e and ν x optical depths but it can be as high as ∼ 5. The results of this work are a first step toward the analysis of neutrino oscillations in a novel astrophysical context and, as such, deserve further attention.

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“…To date, the study, development, and production of medical materials and specifically implants are the most actual issues for materials specialists, chemists, and process engineers [9][10][11][12][13][14][15]. Current trends in the development of high-end technology and laboratory facilities of scientific centers require to enhance the processing techniques for medical goods and extent the product range corresponding to the international standards, along with steady effort to cost reduction [16][17][18].…”

Section: Introductionmentioning

confidence: 99%

Carbonate hydroxylapatite synthesis and crystallization on metallic implants

2014

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The work deals with the synthesis of carbonate hydroxylapatite from a prototype human synovial fluid. The process of carbonate hydroxylapatite crystallization on the alloys of different composition, roughness, and treatment techniques is studied. The quantitative characteristics measuring the efficiency of coating deposition by biomimetic synthesis from the model solution of human synovial fluid are calculated.

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Neutrino oscillations and the early universe

Cited by 6 publications

References 75 publications

Neutrino Oscillations in Neutrino-Dominated Accretion Around Rotating Black Holes

Neutrino Oscillations in Neutrino-Dominated Accretion Around Rotating Black Holes

Neutrino oscillations in a neutrino-dominated accretion disk around a Kerr BH

Carbonate hydroxylapatite synthesis and crystallization on metallic implants

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