Neutrino flavor oscillations in a curved space-time

Visinelli, Luca

doi:10.1007/s10714-015-1899-z

Cited by 47 publications

(30 citation statements)

References 41 publications

(45 reference statements)

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“…Our approach, indeed, once extended to the fermionic case, and in particular to neutrino fields, may give new insights into the existing formalisms dealing with this topic [9,11,13,14]. Moreover, the problems of the phase shift between two neutrino mass eigenstates [11,15,34] and neutrino spin oscillations in gravitational fields [35] could be investigated. Analyzing field mixing in an accelerated frame may serve as a basis for studying a number of other theoretical problems appearing in such a framework.…”

Section: Discussionmentioning

confidence: 91%

Nonthermal signature of the Unruh effect in field mixing

2017

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Mixing transformations for a uniformly accelerated observer (Rindler observer) are analyzed within the quantum field theory framework as a basis for investigating gravitational effects on flavor oscillations. In particular, the case of two charged boson fields with different masses is discussed.In spite of such a minimal setting, the standard Unruh radiation is found to loose its characteristic thermal interpretation due to the interplay between the Bogolubov transformation hiding in field mixing and the one arising from the Rindler spacetime structure. The modified spectrum detected by the Rindler observer is explicitly calculated in the limit of small mass difference.

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Section: Discussionmentioning

confidence: 91%

Nonthermal signature of the Unruh effect in field mixing

2017

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“…Here, the normalized expansion rate 3 The value 0.06 eV is the minimal neutrino mass sum allowed within the normal ordering [282], which is mildly favoured by current data [283][284][285][286]. Leaving the neutrino mass as a free parameter would not change our analysis substantially, given the current very tight upper limits on the sum of the neutrino masses [5,283,[287][288][289][290][291][292][293].…”

Section: Overview Of Models and Model Comparisonmentioning

confidence: 96%

Revisiting a Negative Cosmological Constant from Low-Redshift Data

2019

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Persisting tensions between high-redshift and low-redshift cosmological observations suggest the dark energy sector of the Universe might be more complex than the positive cosmological constant of the ΛCDM model. Motivated by string theory, wherein symmetry considerations make consistent AdS backgrounds (i.e. maximally symmetric spacetimes with a negative cosmological constant) ubiquitous, we explore a scenario where the dark energy sector consists of two components: a negative cosmological constant, with a dark energy component with equation of state w φ on top. We test the consistency of the model against low-redshift Baryon Acoustic Oscillation and Type Ia Supernovae distance measurements, assessing two alternative choices of distance anchors: the sound horizon at baryon drag determined by the Planck collaboration, and the Hubble constant determined by the SH0ES program. We find no evidence for a negative cosmological constant, and mild indications for an effective phantom dark energy component on top. A model comparison analysis reveals the ΛCDM model is favoured over our negative cosmological constant model. While our results are inconclusive, should low-redshift tensions persist with future data, it would be worth reconsidering and further refining our toy negative cosmological constant model by considering realistic string constructions.tions between dark matter particles, or between dark matter and baryons, could alleviate these issues (see e.g. [17][18][19][20][21][22][23][24][25][26][27][28][29][30][31] for an incomplete list of proposed models).

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“…[7,8], was further used in Refs. [9,10] to study neutrino flavor oscillations in static gravitational backgrounds such as Schwarzchild and Kerr metrics.…”

Section: Introductionmentioning

confidence: 99%

“…2, we adapt the formalism for the description of neutrino flavor oscillations, developed in Refs. [7][8][9][10], to describe the neutrino interaction with a time dependent gravitational field, such as GW. Using the solution of the Hamilton-Jacobi equation for a massive particle in GW, previously obtained in Ref.…”

Section: Introductionmentioning

confidence: 99%

Neutrino flavor oscillations in stochastic gravitational waves

Dvornikov

2019

Phys. Rev. D

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We study neutrino flavor oscillations in a plane gravitational wave (GW) with circular polarization. For this purpose we use the solution of the Hamilton-Jacobi equation to get the contribution of GW to the effective Hamiltonian for the neutrino mass eigenstates. Then, considering stochastic GWs, we derive the equation for the density matrix for flavor neutrinos and analytically solve it in the two flavors approximation. We predict the ratios of fluxes of different flavors at a detector for cosmic neutrinos with relatively low energies owing to the interaction with such a GW background. The obtained result is compared with the recent observation of the flavor content of the astrophysical neutrinos fluxes. * maxdvo@izmiran.ru

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Neutrino flavor oscillations in a curved space-time

Cited by 47 publications

References 41 publications

Nonthermal signature of the Unruh effect in field mixing

Nonthermal signature of the Unruh effect in field mixing

Revisiting a Negative Cosmological Constant from Low-Redshift Data

Neutrino flavor oscillations in stochastic gravitational waves

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