Effect of transition magnetic moments on collective supernova neutrino oscillations

Gouvêa, André de; Shalgar, Shashank

doi:10.1088/1475-7516/2012/10/027

Cited by 67 publications

(74 citation statements)

References 61 publications

(112 reference statements)

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“…The spin components which are ignored here, i.e., positive helicity neutrinos, and negative helicity antineutrinos come into play in a number of situations. For example, a strong magnetic field may flip the neutrino helicity and the resulting effect may be amplified by the nonlinear nature of collective oscillations [58][59][60] Even without any magnetic fields, many-body correlations may develop between right and wrong helicity states in the presence of a net flow in the matter background as is the case in an exploding supernova [52,61]. However, these effects are outside of the scope of this paper.…”

Section: A Isospin Operatorsmentioning

confidence: 93%

Neutrino spectral split in the exact many-body formalism

et al. 2018

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We consider the many-body system of neutrinos interacting with each other through neutral current weak force. Emerging many-body effects in such a system could play important roles in some astrophysical sites such as the core collapse supernovae. In the literature this many-body system is usually treated within the mean field approximation which is an effective one-body description based on omitting entangled neutrino states. In this paper, we consider the original many-body system in an effective two flavor mixing scenario under the single angle approximation and present a solution without using the mean field approximation. Our solution is formulated around a special class of many-body eigenstates which do not undergo any level crossings as the neutrino self-interaction rate decreases while the neutrinos radiate from the supernova. In particular, an initial state which consists of electron neutrinos and antineutrinos of an orthogonal flavor can be entirely decomposed in terms of those eigenstates. Assuming that the conditions are perfectly adiabatic so that the evolution of these eigenstates follow their variation with the interaction rate, we show that this initial state develops a spectral split at exactly the same energy predicted by the mean field formulation.

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Section: A Isospin Operatorsmentioning

confidence: 93%

Neutrino spectral split in the exact many-body formalism

et al. 2018

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“…Predictions of the DSNB have improved steadily over the years (Krauss et al 1984;Dar 1985;Totani & Sato 1995;Totani et al 1996;Malaney 1997;Hartmann & Woosley 1997;Kaplinghat et al 2000;Ando & Sato 2003;Fukugita & Kawasaki 2003;Strigari et al 2004;Iocco et al 2005;Strigari et al 2005;Lunardini 2006; Daigne et al 2005;Yuksel et al 2006;Horiuchi et al 2009;Lunardini 2009;Lien et al 2010;Keehn & Lunardini 2012;Lunardini & Tamborra 2012;Nakazato 2013;Mathews et al 2014;Yuksel & Kistler 2015;Nakazato et al 2015;Hidaka et al 2016;Priya & Lunardini 2017). The neutrino emission predicted from core-collapse simulations can be fitted by a modified Fermi-Dirac spectrum with a spectral shape parameter (Keil et al 2003;Tamborra et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Diffuse supernova neutrino background from extensive core-collapse simulations of 8–100 M⊙ progenitors

Horiuchi

Sumiyoshi

Nakamura

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We revisit the diffuse supernova neutrino background in light of recent systematic studies of stellar core collapse that reveal the quantitative impacts of the progenitor conditions on the collapse process. In general, the dependence of the core-collapse neutrino emission on the progenitor is not monotonic in progenitor initial mass, but we show that it can, at first order, be characterized by the core compactness. For the first time, we incorporate the detailed variations in the neutrino emission over the entire mass range 8-100M , based on (i) a long-term simulation of the core collapse of a 8.8M ONeMg core progenitor, (ii) over 100 simulations of iron core collapse to neutron stars, and (iii) half a dozen simulations of core collapse to black holes (the "failed channel"). The fraction of massive stars that undergo the failed channel remains uncertain, but in view of recent simulations which reveal high compactness to be conducive to collapse to black holes, we characterize the failed fraction by considering a threshold compactness above which massive stars collapse to black holes and below which the final remnant is a neutron star. We predict that future detections of the diffuse supernova neutrino background may have the power to reveal this threshold compactness, if its value is relatively small as suggested by interpretations of several recent astronomical observations.

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“…Here, we should stress that we investigate oscillations among neutrino states with different helicity but specific flavor. The corresponding transitions with the change of flavor in a magnetic field (spin-flavor oscillations) have long been extensively studied in a number of publications and applied to supernova conditions (see, for instance, [70,71]). Together with purely flavor conversions in matter (the MSW effect) for the conditions of supernovae they have been shown to appear in outer regions with density ρ 10 6 g/cm 3 .…”

Section: Effects Of Neutrino Mixingmentioning

confidence: 99%

Neutrino spin oscillations in polarized matter

2019

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We study the neutrino spin oscillations, i.e., neutrino spin precession caused by the neutrino interaction with matter polarized by external magnetic field (or, equivalently, by the interaction of the induced magnetic moment (IMM) of a neutrino with the magnetic field). In the analysis, we consider realistic conditions inside supernovae and discuss both the Dirac and Majorana cases. We show that due to the interaction with the polarized matter a neutrino flux from a supernova suffers additional attenuation at low neutrino energies. Another possible effect is that when taken together the effects of conventional magnetic moment and polarized matter can cancel each other so that under certain condition the oscillations disappear. We note that this can lead to the appearance of a characteristic maximum in the spectrum of electron neutrinos from supernovae. Accounting for neutrino mixing (in the two-flavor approximation) can significantly increase (almost twice) the effective value of the IMM of the electron neutrino. As a result, electron neutrinos with twice as high energy will be able to participate in the processes of spin conversion. Various feedback mechanisms accompanying the considered phenomena are also discussed.

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Effect of transition magnetic moments on collective supernova neutrino oscillations

Cited by 67 publications

References 61 publications

Neutrino spectral split in the exact many-body formalism

Neutrino spectral split in the exact many-body formalism

Diffuse supernova neutrino background from extensive core-collapse simulations of 8–100 M⊙ progenitors

Neutrino spin oscillations in polarized matter

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