Consequences of large<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msub><mml:mi>θ</mml:mi><mml:mn>13</mml:mn></mml:msub></mml:math>for the turbulence signatures in supernova neutrinos

Kneller, James P.; Mauney, Alex

doi:10.1103/physrevd.88.025004

Cited by 19 publications

(37 citation statements)

References 70 publications

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“…for |k z | ≥ k ⋆ which is exactly the same as the onedimensional spectrum used in Kneller & Mauney [41]. There is no analytic formula for the two-point structure function for randomly orientated separations using this power spectrum but if we consider the two-point structure function of the random field for points orientated along the z direction then we can compute that in this direction…”

Section: A the Power Spectrummentioning

confidence: 91%

“…The z axis of our Cartesian co-ordinate system is aligned with the radial direction of the profile. The profile we adopt is from a This profile is shown in figure (1) and is the same one used in Kneller & Mauney [41]. The figure shows the presence of two shocks: the forward shock at r s and the reverse shock at r r .…”

Section: Description Of the Calculationsmentioning

confidence: 99%

“…λ ij = 1/|δk ij | andλ ij = 1/|δk ij | -where δk ij and δk ij are the differences between the eigenvalues i and j of the neutrinos and antineutrinos respectively. Kneller & Mauney [41] showed the wavelengths in the turbulence region were of order 1 km or greater which is approximately four orders of magnitude smaller than the shock separation. This means we need to pick N d ≥ 4 to cover the necessary decades in k-space.…”

Section: Description Of the Calculationsmentioning

confidence: 99%

“…Our calculations expand upon the work of Kneller & Volpe [39] and Kneller & Mauney [41] upon which we rely heavily for the techniques used to calculate the turbulence effects and as context for our results. We begin by describing the calculations we undertook paying particular attention to the construction of the random fields used to model the turbulence.…”

Section: Introductionmentioning

confidence: 99%

“…It has been shown that the transition probabilities for a single neutrino -the set of probabilities that relates the initial state to the state after passing through the supernova -is not unique when turbulence is inserted into a profile: it will depend upon the exact turbulence pattern seen by the neutrino as it travelled through the supernova [38,39,41]. Those transition probabilities are drawn from distributions whose properties will depend upon the stage of the explosion, the character of the turbulence, and the neutrino energy and mixing parameters.…”

Section: Introductionmentioning

confidence: 99%

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Does the finite size of the proto-neutron star preclude supernova neutrino flavor scintillation due to turbulence?

Kneller

Mauney

2013

Phys. Rev. D

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The transition probabilities describing the evolution of a neutrino with a given energy along some ray through a turbulent supernova are random variates unique to each ray. If the source of the neutrinos were a point then all neutrinos of a given energy and emitted at the same time which were detected in some far off location would have seen the same turbulent profile therefore their transition probabilities would be exactly correlated and would not form a representative sample of the underlying parent transition probability distributions. But if the source has a finite size then the profiles seen by neutrinos emitted from different points at the source will have seen different turbulence and the correlation of the transition probabilities will be reduced. In this paper we study the correlation of the neutrino transition probabilities through turbulent supernova profiles as a function of the separation δx between the emission points using an isotropic and an anisotropic power spectrum for the random field used to model the turbulence. We find that if we use an isotropic power spectrum for the random field, the correlation of the high (H) density resonance mixing channel transition probability is significant, greater than 0.5, for emission separations of δx = 10 km, typical of proto neutron star radii, only when the turbulence amplitude is less than C⋆ ∼ 10%; at larger amplitudes the correlation in this channel drops close to zero for this same separation of δx = 10 km. In contrast, there is significant correlation in the low (L) density resonant and non-resonant channels even for turbulence amplitudes as high as 50%. Switching to anisotropic spectra requires the introduction of an 'isotropy' parameter kI whose inverse defines the scale below which the field is isotropic. We find the correlation of all transition probabilities, especially the H resonance channel, strongly depends upon the choice of kI relative to the long wavelength radial cutoff k⋆. The spectral features in the H resonance mixing channel of the next Galactic supernova neutrino burst may be strongly obscured by large amplitude turbulence when it enters the signal due to the finite size of the source while the presence of features in the L and non resonant mixing channels may persist, the exact amount depending upon the degree of anisotropy of the turbulence.

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Section: A the Power Spectrummentioning

confidence: 91%

Section: Description Of the Calculationsmentioning

confidence: 99%

Section: Description Of the Calculationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Does the finite size of the proto-neutron star preclude supernova neutrino flavor scintillation due to turbulence?

Kneller

Mauney

2013

Phys. Rev. D

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Turbulence and its effects upon neutrinos

Kneller¹,

McLaughlin²,

Patton³

2014

AIP Conference Proceedings

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As a neutrino passes through turbulent matter, large amplitude transitions between its eigenstates can occur. These transitions can be modeled as like those of an irradiated polarized atom and we investigate this connection both analytically and numerically. We find a simple theory that makes use of the Rotating Wave Approximation can make predictions for the amplitudes and wavelengths of the transitions that agree very well with those from the numerical solutions.

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A New Multi-Dimensional General Relativistic Neutrino Hydrodynamics Code for Core-Collapse Supernovae. Iv. The Neutrino Signal

Müller

Janka

2014

ApJ

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Considering six general relativistic, two-dimensional (2D) supernova (SN) explosion models of progenitor stars between 8.1 and 27 M ⊙ , we systematically analyze the properties of the neutrino emission from core collapse and bounce to the post-explosion phase. The models were computed with the Vertex-CoCoNuT code, using three-flavor, energy-dependent neutrino transport in the ray-by-ray-plus approximation. Our results confirm the close similarity of the mean energies, E , ofν e and heavy-lepton neutrinos and even their crossing during the accretion phase for stars with M 10 M ⊙ as observed in previous 1D and 2D simulations with stateof-the-art neutrino transport. We establish a roughly linear scaling of Eν e with the proto-neutron star (PNS) mass, which holds in time as well as for different progenitors. Convection inside the PNS affects the neutrino emission on the 10-20% level, and accretion continuing beyond the onset of the explosion prevents the abrupt drop of the neutrino luminosities seen in artificially exploded 1D models. We demonstrate that a waveletbased time-frequency analysis of SN neutrino signals in IceCube will offer sensitive diagnostics for the SN core dynamics up to at least ∼10 kpc distance. Strong, narrow-band signal modulations indicate quasi-periodic shock sloshing motions due to the standing accretion shock instability (SASI), and the frequency evolution of such "SASI neutrino chirps" reveals shock expansion or contraction. The onset of the explosion is accompanied by a shift of the modulation frequency below 40-50 Hz, and post-explosion, episodic accretion downflows will be signaled by activity intervals stretching over an extended frequency range in the wavelet spectrogram.

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Consequences of largeθ13for the turbulence signatures in supernova neutrinos

Cited by 19 publications

References 70 publications

Does the finite size of the proto-neutron star preclude supernova neutrino flavor scintillation due to turbulence?

Does the finite size of the proto-neutron star preclude supernova neutrino flavor scintillation due to turbulence?

Turbulence and its effects upon neutrinos

A New Multi-Dimensional General Relativistic Neutrino Hydrodynamics Code for Core-Collapse Supernovae. Iv. The Neutrino Signal

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