Astrophysical Axion Bounds

Raffelt, Georg G.

doi:10.1007/978-3-642-56643-1_8

Cited by 121 publications

(206 citation statements)

References 66 publications

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“…We now discuss weak magnetism and recoil corrections to the emitted ν x andν x spectra. We will use a simple Monte Carlo model of Raffelt [25] to estimate the emitted spectra. We emphasize that this simple model should be checked against full simulations that include weak magnetism and recoil.…”

Section: Spectrummentioning

confidence: 99%

“…We consider the following simple model [25] to estimate the change in theν e spectrum with weak magnetism. Let theν e neutrino sphere be at a temperature T 0 without weak magnetism.…”

Section: B Spectrum Ofνementioning

confidence: 99%

“…The extra -1 in the denominator follows because the optical depth involves a path integral from the neutrino sphere to infinity [25]. Realistic values of u could be ∼ 0.25 to 0.35 [25]. The energy dependent temperature T (k) defines the emitted spectrum, …”

Section: B Spectrum Ofνementioning

confidence: 99%

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Weak magnetism for antineutrinos in supernovae

2002

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Weak magnetism increases antineutrino mean free paths in core collapse supernovae. The parity violating interference between axial and vector currents makes antineutrino-nucleon cross sections smaller then those for neutrinos. We calculate simple, exact correction factors to include recoil and weak magnetism in supernova simulations. Weak magnetism may significantly increase the neutrino energy flux. We calculate, in a diffusion approximation, an increase of order 15% in the total energy flux for temperatures near 10 MeV. This should raise the neutrino luminosity. Weak magnetism also changes the emitted spectrum ofνx (with x = µ or τ ) andνe. We estimate thatνx will be emitted about 7% hotter than νx becauseνx have longer mean free paths. Likewise weak magnetism may increase theνe temperature by of order 10%. This increase in temperature coupled with the increase in neutrino luminosity should increase the heating in the low density region outside of the neutrino sphere. This, in turn, could be important for the success of an explosion. It is important to check our results with a full simulation that includes Boltzmann neutrino transport and weak magnetism corrections.

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Section: Spectrummentioning

confidence: 99%

“…We consider the following simple model [25] to estimate the change in theν e spectrum with weak magnetism. Let theν e neutrino sphere be at a temperature T 0 without weak magnetism.…”

Section: B Spectrum Ofνementioning

confidence: 99%

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Weak magnetism for antineutrinos in supernovae

2002

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“…Supernova (SN) neutrinos continue to be a subject of great interest in astroparticle physics [1]. In particular, renewed attention is being paid to collective features of flavor transformations induced by ν (ν) self-interactions (see [2] and refs.…”

Section: Introductionmentioning

confidence: 99%

Low-energy spectral features of supernova (anti)neutrinos in inverted hierarchy

et al. 2008

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In the dense supernova core, self-interactions may align the flavor polarization vectors of ν and ν, and induce collective flavor transformations. Different alignment ansatzes are known to describe approximately the phenomena of synchronized or bipolar oscillations, and the split of ν energy spectra. We discuss another phenomenon observed in some numerical experiments in inverted hierarchy, showing features akin to a low-energy split of ν spectra. The phenomenon appears to be approximately described by another alignment ansatz which, in the considered scenario, reduces the (nonadiabatic) dynamics of all energy modes to only two ν plus two ν modes. The associated spectral features, however, appear to be fragile when passing from single-to multi-angle simulations.

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“…Current status is reviewed by many authors. 7,8) In such present situation, much attention have been paid to another neutrino source, supernova. This is a completely different system from sun, atmosphere, accelerator, and reactor in regard to neutrino energy, flavor of produced neutrinos, propagation length and so forth.…”

Section: Introductionmentioning

confidence: 99%

Neutrino Burst from Supernovae and Neutrino Oscillation

2008

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Core-collapse driven supernovae are the most luminous neutrino source in the universe. SK (SuperKamiokande) and SNO (Sudbury Neutrino Observatory showed that neutrinos have finite masses and convert each other from the solar and atmospheric neutrino observations. The time profile and energy spectrum of neutrino burst from supernovae should be greatly modified by this effect. We review how this conversion happens in a supernova mantle and how the burst will be detected by SK and SNO. We show that implications for neutrino parameters (mass hierarchy and the mixing angle between mass eigenstate 1 , 3 ), are obtained if a supernova appears at Galactic Center. We also discuss effects of neutrino oscillation on the supernova relic neutrino observations.

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Astrophysical Axion Bounds

Cited by 121 publications

References 66 publications

Weak magnetism for antineutrinos in supernovae

Weak magnetism for antineutrinos in supernovae

Low-energy spectral features of supernova (anti)neutrinos in inverted hierarchy

Neutrino Burst from Supernovae and Neutrino Oscillation

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