Higher Order Correction to the Neutrino Self-Energy in a Medium and Its Astrophysical Applications

Garcia, Antonio; Sahu, Sarira

doi:10.1142/s0217732307020865

Cited by 5 publications

(2 citation statements)

References 17 publications

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“…In the absence of magnetic field the neutrino self-energy and the neutrino effective potential is calculated earlier [40]. In this case the neutrino self-energy is decomposed as…”

Section: Neutrino Potential Without Magnetic Fieldmentioning

confidence: 99%

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Propagation of neutrinos through magnetized gamma-ray burst fireball

Sahu

Fraija

Keum

2009

J. Cosmol. Astropart. Phys.

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The neutrino self-energy is calculated in a weakly magnetized plasma consists of electrons, protons, neutrons and their anti-particles and using this we have calculated the neutrino effective potential up to order M −4 W . In the absence of magnetic field it reduces to the known result. We have also calculated explicitly the effective potentials for different backgrounds which may be helpful in different environments. By considering the mixing of three active neutrinos in the medium with the magnetic field we have derived the survival and conversion probabilities of neutrinos from one flavor to another and also the resonance condition is derived. As an application of the above, we considered the dense and relativistic plasma of the Gamma-Ray Bursts fireball through which neutrinos of 5-30 MeV can propagate and depending on the fireball parameters they may oscillate resonantly or nonresonantly from one flavor to another. These MeV neutrinos are produced due to stellar collapse or merger events which trigger the Gamma-Ray Burst. The fireball itself also produces MeV neutrinos due to electron positron annihilation, inverse beta decay and nucleonic bremsstrahlung. Using the three neutrino mixing and considering the best fit values of the neutrino parameters, we found that electron neutrinos are hard to oscillate to another flavors. On the other hand, the muon neutrinos and the tau neutrinos oscillate with equal probability to one another, which depends on the neutrino energy, temperature and size of the fireball. Comparison of oscillation probabilities with and without magnetic field shows that, they depend on the neutrino energy and also on the size of the fireball. By using the resonance condition, we have also estimated the resonance length of the propagating neutrinos as well as the baryon content of the fireball. *

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“…In the absence of magnetic field the neutrino self-energy and the neutrino effective potential is calculated earlier [40]. In this case the neutrino self-energy is decomposed as…”

Section: Neutrino Potential Without Magnetic Fieldmentioning

confidence: 99%

“…This is the result obtained in ref. [40] up to order 1/M 4 W for neutrino propagating in a medium with only electrons and positrons in it.…”

Section: Neutrino Potential Without Magnetic Fieldmentioning

confidence: 99%

Propagation of neutrinos through magnetized gamma-ray burst fireball

Sahu

Fraija

Keum

2009

J. Cosmol. Astropart. Phys.

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Neutrino Self-energy in a Magnetized Charge-symmetric Medium

Garcia¹,

Bhattacharya²,

Sahu³

et al. 2008

AIP Conference Proceedings

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Abstract. In this talk we present the calculation of the neutrino self-energy in presence of a magnetized medium. The magnetized medium consists of electrons, positrons, neutrinos and a uniform classical magnetic field. The background magnetic field is assumed to be weak compared to the W -Boson mass as a consequence of which only linear order corrections in the field are included in the W boson propagator. The electron propagator consists all order corrections in the background field. Our calculation is specifically suited for situations where the background plasma may be CP symmetric.

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Propagation and Neutrino Oscillations in the Base of a Highly Magnetized Gamma-Ray Burst Fireball Flow

Fraija

2014

ApJ

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Neutrons play an important role in the dynamics of gamma-ray bursts. The presence of neutrons in the baryon-loaded fireball is expected. If the neutrons abundance is comparable to that of protons, important features may be observed such as quasithermal multi-GeV neutrinos in coincidence with a subphotospheric γ-ray emission, nucleosynthesis at later times and rebrightening of the afterglow emission. Additionally, thermal MeV neutrinos are created by electron-positron annihilation, electron (positron) capture on protons (neutrons) and nucleonic bremsstrahlung. Although MeV neutrinos are difficult to detect, quasi-thermal GeV neutrinos are expected in km 3 detectors and/or DeepCore+IceCube. In this paper, we show that neutrino oscillations have outstanding implications for the dynamics of the fireball evolution and also that they can be detected through their flavor ratio on Earth. For that we derive the resonance and charged-neutrality conditions as well as the neutrino self-energy and effective potential up to order m −4 W at strong, moderate and weak magnetic field approximation to constrain the dynamics of the fireball. We found important implications: i) resonant oscillations are suppressed for high baryon densities as well as neutrons abundance larger than that of protons and ii) the effect of magnetic field is to decrease the proton-to-neutron ratio aside from the number of multi-GeV neutrinos expected in DeepCore detector. Also we estimate the GeV neutrino flavor ratios along the jet and on Earth.

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Higher Order Correction to the Neutrino Self-Energy in a Medium and Its Astrophysical Applications

Cited by 5 publications

References 17 publications

Propagation of neutrinos through magnetized gamma-ray burst fireball

Propagation of neutrinos through magnetized gamma-ray burst fireball

Neutrino Self-energy in a Magnetized Charge-symmetric Medium

Propagation and Neutrino Oscillations in the Base of a Highly Magnetized Gamma-Ray Burst Fireball Flow

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