Turbulence patterns and neutrino flavor transitions in high-resolution supernova models

Enrico Borriello, Sovan Chakraborty, Hans Thomas Janka, Eligio Lisi, Alessandro Mirizzi

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

During the shock-wave propagation in a core-collapse supernova (SN), matter turbulence may affect neutrino flavor conversion probabilities. Such effects have been usually studied by adding parametrized small-scale random fluctuations (with arbitrary amplitude) on top of coarse, spherically symmetric matter density profiles. Recently, however, two-dimensional (2D) SN models have reached a space resolution high enough to directly trace anisotropic density profiles, down to scales smaller than the typical neutrino oscillation length. In this context, we analyze the statistical properties of a large set of SN matter density profiles obtained in a high-resolution 2D simulation, focusing on a post-bounce time (2 s) suited to study shock-wave effects on neutrino propagation on scales as small as O(100) km and possibly below. We clearly find the imprint of a broken (Kolmogorov-Kraichnan) power-law structure, as generically expected in 2D turbulence spectra. We then compute the flavor evolution of SN neutrinos along representative realizations of the turbulent matter density profiles, and observe no or modest damping of the neutrino crossing probabilities on their way through the shock wave. In order to check the effect of possibly unresolved fluctuations at scales below O(100) km, we also apply a randomization procedure anchored to the power spectrum calculated from the simulation, and find consistent results within ± 1σ fluctuations. These results show the importance of anchoring turbulence effects on SN neutrinos to realistic, fine-grained SN models.

Original languageEnglish (US)
Article number030
JournalJournal of Cosmology and Astroparticle Physics
Volume2014
Issue number11
DOIs
StatePublished - Nov 1 2014
Externally publishedYes

Fingerprint

supernovae
neutrinos
turbulence
high resolution
profiles
shock waves
shock wave propagation
turbulence effects
power spectra
simulation
damping
oscillations
propagation

Keywords

  • Core-collapse supernovas
  • Supernova neutrinos

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Cite this

Turbulence patterns and neutrino flavor transitions in high-resolution supernova models. / Borriello, Enrico; Chakraborty, Sovan; Janka, Hans Thomas; Lisi, Eligio; Mirizzi, Alessandro.

In: Journal of Cosmology and Astroparticle Physics, Vol. 2014, No. 11, 030, 01.11.2014.

Research output: Contribution to journalArticle

Borriello, Enrico ; Chakraborty, Sovan ; Janka, Hans Thomas ; Lisi, Eligio ; Mirizzi, Alessandro. / Turbulence patterns and neutrino flavor transitions in high-resolution supernova models. In: Journal of Cosmology and Astroparticle Physics. 2014 ; Vol. 2014, No. 11.
@article{33fc385edb2f47a5b78fcc9f4d7a1b56,
title = "Turbulence patterns and neutrino flavor transitions in high-resolution supernova models",
abstract = "During the shock-wave propagation in a core-collapse supernova (SN), matter turbulence may affect neutrino flavor conversion probabilities. Such effects have been usually studied by adding parametrized small-scale random fluctuations (with arbitrary amplitude) on top of coarse, spherically symmetric matter density profiles. Recently, however, two-dimensional (2D) SN models have reached a space resolution high enough to directly trace anisotropic density profiles, down to scales smaller than the typical neutrino oscillation length. In this context, we analyze the statistical properties of a large set of SN matter density profiles obtained in a high-resolution 2D simulation, focusing on a post-bounce time (2 s) suited to study shock-wave effects on neutrino propagation on scales as small as O(100) km and possibly below. We clearly find the imprint of a broken (Kolmogorov-Kraichnan) power-law structure, as generically expected in 2D turbulence spectra. We then compute the flavor evolution of SN neutrinos along representative realizations of the turbulent matter density profiles, and observe no or modest damping of the neutrino crossing probabilities on their way through the shock wave. In order to check the effect of possibly unresolved fluctuations at scales below O(100) km, we also apply a randomization procedure anchored to the power spectrum calculated from the simulation, and find consistent results within ± 1σ fluctuations. These results show the importance of anchoring turbulence effects on SN neutrinos to realistic, fine-grained SN models.",
keywords = "Core-collapse supernovas, Supernova neutrinos",
author = "Enrico Borriello and Sovan Chakraborty and Janka, {Hans Thomas} and Eligio Lisi and Alessandro Mirizzi",
year = "2014",
month = "11",
day = "1",
doi = "10.1088/1475-7516/2014/11/030",
language = "English (US)",
volume = "2014",
journal = "Journal of Cosmology and Astroparticle Physics",
issn = "1475-7516",
publisher = "IOP Publishing Ltd.",
number = "11",

}

TY - JOUR

T1 - Turbulence patterns and neutrino flavor transitions in high-resolution supernova models

AU - Borriello, Enrico

AU - Chakraborty, Sovan

AU - Janka, Hans Thomas

AU - Lisi, Eligio

AU - Mirizzi, Alessandro

PY - 2014/11/1

Y1 - 2014/11/1

N2 - During the shock-wave propagation in a core-collapse supernova (SN), matter turbulence may affect neutrino flavor conversion probabilities. Such effects have been usually studied by adding parametrized small-scale random fluctuations (with arbitrary amplitude) on top of coarse, spherically symmetric matter density profiles. Recently, however, two-dimensional (2D) SN models have reached a space resolution high enough to directly trace anisotropic density profiles, down to scales smaller than the typical neutrino oscillation length. In this context, we analyze the statistical properties of a large set of SN matter density profiles obtained in a high-resolution 2D simulation, focusing on a post-bounce time (2 s) suited to study shock-wave effects on neutrino propagation on scales as small as O(100) km and possibly below. We clearly find the imprint of a broken (Kolmogorov-Kraichnan) power-law structure, as generically expected in 2D turbulence spectra. We then compute the flavor evolution of SN neutrinos along representative realizations of the turbulent matter density profiles, and observe no or modest damping of the neutrino crossing probabilities on their way through the shock wave. In order to check the effect of possibly unresolved fluctuations at scales below O(100) km, we also apply a randomization procedure anchored to the power spectrum calculated from the simulation, and find consistent results within ± 1σ fluctuations. These results show the importance of anchoring turbulence effects on SN neutrinos to realistic, fine-grained SN models.

AB - During the shock-wave propagation in a core-collapse supernova (SN), matter turbulence may affect neutrino flavor conversion probabilities. Such effects have been usually studied by adding parametrized small-scale random fluctuations (with arbitrary amplitude) on top of coarse, spherically symmetric matter density profiles. Recently, however, two-dimensional (2D) SN models have reached a space resolution high enough to directly trace anisotropic density profiles, down to scales smaller than the typical neutrino oscillation length. In this context, we analyze the statistical properties of a large set of SN matter density profiles obtained in a high-resolution 2D simulation, focusing on a post-bounce time (2 s) suited to study shock-wave effects on neutrino propagation on scales as small as O(100) km and possibly below. We clearly find the imprint of a broken (Kolmogorov-Kraichnan) power-law structure, as generically expected in 2D turbulence spectra. We then compute the flavor evolution of SN neutrinos along representative realizations of the turbulent matter density profiles, and observe no or modest damping of the neutrino crossing probabilities on their way through the shock wave. In order to check the effect of possibly unresolved fluctuations at scales below O(100) km, we also apply a randomization procedure anchored to the power spectrum calculated from the simulation, and find consistent results within ± 1σ fluctuations. These results show the importance of anchoring turbulence effects on SN neutrinos to realistic, fine-grained SN models.

KW - Core-collapse supernovas

KW - Supernova neutrinos

UR - http://www.scopus.com/inward/record.url?scp=84914151100&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84914151100&partnerID=8YFLogxK

U2 - 10.1088/1475-7516/2014/11/030

DO - 10.1088/1475-7516/2014/11/030

M3 - Article

AN - SCOPUS:84914151100

VL - 2014

JO - Journal of Cosmology and Astroparticle Physics

JF - Journal of Cosmology and Astroparticle Physics

SN - 1475-7516

IS - 11

M1 - 030

ER -