Runaway stars as cosmic ray injectors inside molecular clouds

TL;DR

This paper models how runaway stars within giant molecular clouds accelerate particles at bowshocks, producing non-thermal emissions in radio, X-ray, and gamma-ray wavelengths, contributing to the understanding of cosmic ray sources.

Contribution

It introduces a new model for non-thermal radiation from protons and secondary pairs accelerated by runaway stars' bowshocks inside GMCs, linking stellar dynamics to cosmic ray injection.

Findings

X-ray luminosities around 10^32 erg/s

Gamma-ray luminosities around 10^34 erg/s

Extended non-thermal sources from runaway star interactions

Abstract

Giant molecular clouds (GMCs) are a new population of gamma-ray sources, being the target of cosmic rays (CRs) -- locally accelerated or not --. These clouds host very young stellar clusters where massive star formation takes place. Eventually, some of the stars are ejected from the clusters, becoming runaway stars. These stars move supersonically through the cloud and develop bowshocks where particles can be accelerated up to relativistic energies. As a result, the bowshocks present non-thermal emission, and inject relativistic protons in the cloud. These protons diffuse in the GMC interacting with the matter. We present a model for the non-thermal radiation generated by protons and secondary pairs accelerated in the bowshocks of massive runaways stars within young GMCs. We solve the transport equation for primary protons and secondary pairs as the stars move through the cloud. We present non-thermal emissivity maps in radio and in gamma rays as a function of time. We obtain X-ray luminosities of the order $\sim$ ${ 10^{32}}$ erg~s$^{-1}$ and gamma-ray luminosities $\sim$ $10^{34}$ erg~s$^{-1}$. We conclude that, under some assumptions, relativistic protons from massive runaway stars interacting with matter in GMCs give rise to extended non-thermal sources.