Energy losses of a neutron star due to inverse muon decay in the superstrong magnetic field

Likhachev, G. G.; Studenikin, A. I.

doi:10.1007/bf00560269

Cited by 11 publications

(25 citation statements)

References 7 publications

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“…However, these transitions are still independent from the neutrino energy, which does not enter in the evolution equation (158).…”

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

“…Considering Dirac neutrinos, which can have diagonal magnetic moments µ ee and µ µµ , as well as transition magnetic moments µ eµ and µ µe , the evolution equation of the amplitudes, obtained by combining Eqs. (48) and (158) and neglecting irrelevant diagonal terms, is cos 2ϑ…”

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

“…A realization of the second resonance requires a large neutron number density, as that in a neutron star. The neutrino spin oscillations in a transverse magnetic field with a possible rotation of the field-strength vector in a plane orthogonal to the neutrino-propagation direction (such rotating fields may exist in the convective zone of the Sun) have been considered in [158,161]. The effect of the magnetic-field rotation may substantially shift the resonance point of neutrino oscillations.…”

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

“…It is possible to formulate a criterion [158] for finding out if the neutrino spin (spinflavor) precession is significant for given neutrino and background medium properties. The probability of oscillatory transitions between two neutrino states ν αL ⇆ ν βR can be expressed in terms of the elements of the effective Hamiltonian matrices (167) and (170) as …”

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

“…that the neutrino spin-flip transitions in a magnetic field provide an efficient mechanism of energy transfer from a protoneutron star, was first discussed in [174] and then investigated [175] in some detail. The possibility of a loss of up to half of the active left-handed neutrinos because of their transition to sterile right-handed neutrinos in strong magnetic fields at the boundary of the neutron star (the so-called boundary effect) was considered in [158].…”

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

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Neutrino electromagnetic properties

2009

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The main goal of the paper is to give a short review on neutrino electromagnetic properties. In the introductory part of the paper a summary on what we really know about neutrinos is given: we discuss the basics of neutrino mass and mixing as well as the phenomenology of neutrino oscillations. This is important for the following discussion on neutrino electromagnetic properties that starts with a derivation of the neutrino electromagnetic vertex function in the most general form, that follows from the requirement of Lorentz invariance, for both the Dirac and Majorana cases. Then, the problem of the neutrino form factors definition and calculation within gauge models is considered. In particular, we discuss the neutrino electric charge form factor and charge radius, dipole magnetic and electric and anapole form factors. Available experimental constraints on neutrino electromagnetic properties are also discussed, and the recently obtained experimental limits on neutrino magnetic moments are reviewed. The most important neutrino electromagnetic processes involving a direct neutrino coupling with photons (such as neutrino radiative decay, neutrino Cherenkov radiation, spin light of neutrino and plasmon decay into neutrino-antineutrino pair in media) and neutrino resonant spin-flavor precession in a magnetic field are discussed at the end of the paper.

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“…However, these transitions are still independent from the neutrino energy, which does not enter in the evolution equation (158).…”

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

Section: Neutrino Spin-flavor Precession In Magnetic Fieldmentioning

confidence: 99%

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Neutrino electromagnetic properties

2009

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Neutrino self-polarization effect in matter

Lobanov

Studenikin

2004

Physics Letters B

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The quasi-classical theory of the spin light of neutrino (SLν) in background matter, accounting for the neutrino polarization, is developed. The neutrino transitions ν L → ν R and ν R → ν L rates in matter are calculated. It is shown that the SLν in matter leads to the neutrino conversion from active ν L to sterile ν R states (neutrino self-polarization effect in matter).Convincing evidence in favour of non-zero neutrino mass that has been obtained during the last few years in atmospheric and solar-neutrino experiments, are also confirming in the reactor KamLAND and long-baseline accelerator experiments (see [1] for a review on the present status of neutrino mixing and oscillations). Even within the standard model (minimally extended with SU(2)−singlet right-handed neutrino) a massive neutrino inevitably has non-zero magnetic moment µ generated by the one-loop diagramme [2]. A recent studies of a massive neutrino electromagnetic properties within one-loop level, including discussion on the neutrino magnetic moment, can be found in [3]. It should be also noted here that a rather detailed discussion on the neutrino charge radius is presented in the two recent papers [4,5].In a series of our papers [6][7][8][9][10][11] we have developed the Lorentz invariant approach to neutrino oscillations which enables us to study, in particular, the neutrino spin procession in the background matter with effects of the presence of electromagnetic and gravitational fields being also accounted for. A review on these our studies can be found in [12]. * E-mail: studenik@srd.sinp.msu.ru 1 In [10,11] we have predicted the new mechanism of electromagnetic radiation by neutrino moving in background matter and/or electromagnetic and gravitational fields. We have named this radiation as "spin light of neutrino" and introduced the abbreviation SLν which we shall use below in this paper. The SLν originates from the neutrino spin precession that can be induced whether by weak interactions of neutrino with the background matter or by the external electromagnetic or gravitational fields that could be present in the background environment. It should be noted that the discussed mechanism of electromagnetic radiation by a neutrino moving in a constant magnetic field was also studied previously in [13].As we have shown in [10], the total power of the SLν in matter does not washed out when the emitted photon refractive index is equal to unit and the SLν can not be considered as the neutrino Cerenkov radiation (see, for example, [14] and references therein). It was also emphasized [10] that the initially unpolarized neutrino beam (equal mixture of active left-handed and sterile right-handed neutrinos) can be converted to the totally polarized beam composed of only ν R due to the spin light in contrast to the Cherenkov radiation which can not produce the neutrino spin self-polarization effect.The discovered important properties of SLν (such as strong beaming of the radiation along the neutrino momentum, the rapid growth of the total radiation...

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Neutrino oscillations in electromagnetic fields

2000

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Oscillations of neutrinos ν L ↔ ν R in presence of an arbitrary electromagnetic field are considered. We introduce the Hamiltonian for the neutrino spin evolution equation that accounts for possible effects of interaction of neutrino magnetic µ and electric ǫ dipole moments with the transversal (in respect to the neutrino momentum) and also the longitudinal components of electromagnetic field. Using this Hamiltonian we predict the new types of resonances in the neutrino oscillations ν L ↔ ν R in the presence of the field of an electromagnetic wave and in combination of an electromagnetic wave and constant magnetic field. The possible influence of the longitudinal magnetic field on neutrino oscillations is emphasized.The electromagnetic properties of neutrinos are among the most interesting issues in particle physics. Studies of the neutrino electromagnetic properties could provide an important information about the structure of theoretical model of particle interaction. For instance, the discovery of the non-vanishing neutrino magnetic moment, as well as the neutrino mass, would clearly indicate that the Standard Model has to be generalized.The non-vanishing neutrino magnetic moment has also crucial consequences in astrophysics. As it has been shown in plenty of studies (see, for example, [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18]) that have emerged during past decades, the neutrino conversions and oscillations produced under the influence of transversal constant or constant and twisting (in space) magnetic fields could be important for evolution of astrophysical object, like the Sun and neutron stars, or could result in sufficient effects while neutrinos propagate through interstellar galactic media 2 .In the previously performed studies of neutrino spin precession only effects of the neutrino magnetic (or flavour transition) moment interaction 1 E-mail: studenik@srdlan.npi.msu.su 2 It should be noted here that the neutrino helicity flip could be caused not only by the interaction with an external magnetic field (or, as it is shown below with an electromagnetic wave) but also by the scattering with charged fermions in the background (see, for example, [19] and references therein)

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Energy losses of a neutron star due to inverse muon decay in the superstrong magnetic field

Cited by 11 publications

References 7 publications

Neutrino electromagnetic properties

Neutrino electromagnetic properties

Neutrino self-polarization effect in matter

Neutrino oscillations in electromagnetic fields

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