Loaded layer-cake model for cosmic ray interaction around exploding super-giant stars making black holes

TL;DR

This paper introduces a new cosmic ray interaction model involving supergiant star environments, explaining observed spectra and flux reductions below 100 GV, and accounting for secondary particles and high-energy phenomena.

Contribution

The paper presents a novel layered model of cosmic ray interactions around supergiant stars, improving explanations of observed spectra and secondary particle ratios.

Findings

Model matches AMS cosmic ray data below 100 GV

Predicts secondary/primary ratio slope of -1/3

Accounts for cosmic ray anti-protons, gamma rays, and neutrinos

Abstract

The AMS experiment on the International Space Station has provided detailed cosmic ray spectra for various elements, revealing that interactions significantly reduce fluxes up to about 100 GV rigidity. This necessitates revisiting current cosmic ray interaction models. A new model proposed here involves cosmic ray interactions first in the wind shock shell of supergiant stars and second in the OB-Superbubble around supernovae. These stars, including red and blue supergiants, produce black holes and drive electric currents in winds and jets. Variability in these winds creates temporary electric fields that accelerate particles, resulting in steep spectra with synchrotron losses, and analogous hadron spectra produce a flat magnetic irregularity spectrum. This model matches AMS data, explaining cosmic ray spectra below 100 GV. The model predicts a secondary/primary ratio slope of -1/3 and a primary flux reduction below 100 GV relative to a power-law spectrum with slope +2. Key aspects are: a larger interaction column due to heavy element enrichment and a minor secondary contribution even for elements like He, C, and O, as indicated by the $^3$He/$^4$He ratio. This model also accounts for cosmic ray anti-protons, gamma-ray spectra, and high-energy neutrinos, including contributions from ISM-SNe.