Flavor composition of supernova neutrinos

Predicting the flavor composition of neutrinos from supernovae is a challenging task, primarily due to the high neutrino densities at their core. In such an environment, neutrino self-interactions give rise to collective effects that have dramatic yet poorly understood consequences for their flavor evolution. In this paper, however, we show that standard matter effects in the outer layers of supernovae can significantly constrain the flavor composition of the neutrino flux. We assume that, since a large number of neutrinos undergo different evolutions within the core, their state upon entering the Mikheyev–Smirnov–Wolfenstein-dominated region is affected by decoherence. This assumption simplifies the problem and suggests that the fraction of neutrinos with electron flavor reaching Earth, denoted as <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:msub><a:mi>f</a:mi><a:msub><a:mi>ν</a:mi><a:mi>e</a:mi></a:msub></a:msub></a:math>, is constrained to be less than 0.5 for all energies throughout the emission phase in the case of normal mass ordering. In contrast, for inverted mass ordering, we anticipate neutrinos arriving in near flavor equipartition (<c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:msub><c:mi>f</c:mi><c:msub><c:mi>ν</c:mi><c:mi>e</c:mi></c:msub></c:msub><c:mo>≈</c:mo><c:mn>1</c:mn><c:mo>/</c:mo><c:mn>3</c:mn></c:math>). These predictions, and consequently their underlying assumptions, could be tested by future observations and may provide valuable insights into the properties of neutrino fluxes emerging from supernovae.