High-Energy Neutrino Flavor State Transition Probabilities

TL;DR

This paper analytically calculates neutrino flavor transition probabilities from various astrophysical sources, including higher-order transitions, to understand neutrino behavior over cosmic distances.

Contribution

It introduces an analytical method for determining high-energy neutrino transition probabilities, including higher-order states beyond the Standard Model.

Findings

Calculated approximate cross sections for high-energy neutrinos.

Compared flavor distributions from different astrophysical sources.

Analyzed higher-order neutrino transition probabilities.

Abstract

We analytically determine neutrino transitional probabilities and abundance ratios at various distances from the source of creation in several astrophysical contexts, including the Sun, supernovae and cosmic rays. In doing so, we determine the probability of a higher-order transition state from $\nu_\tau\rightarrow\nu_\lambda$, where $\nu_\lambda$ represents a more massive generation than Standard Model neutrinos. We first calculate an approximate cross section for high-energy neutrinos which allows us to formulate comparisons for the oscillation distances of solar, supernova and higher-energy cosmic ray neutrinos. The flavor distributions of the resulting neutrino populations from each source detected at Earth are then compared via fractional density charts.