Cosmic-ray ionization of molecular clouds

TL;DR

This study investigates the role of low-energy cosmic rays, which are difficult to measure directly, in ionizing molecular clouds, and finds that a significant low-energy component of cosmic rays is needed to explain observed ionization rates.

Contribution

The paper provides a comprehensive analysis of low-energy cosmic-ray spectra and their impact on molecular cloud ionization, highlighting the importance of electrons in this process.

Findings

Low-energy cosmic rays are essential for explaining ionization rates in molecular clouds.

Models with increased low-energy electron flux match observational data.

A significant low-energy component of cosmic rays likely exists in the interstellar medium.

Abstract

Low-energy cosmic rays are a fundamental source of ionization for molecular clouds, influencing their chemical, thermal and dynamical evolution. The purpose of this work is to explore the possibility that a low-energy component of cosmic-rays, not directly measurable from the Earth, can account for the discrepancy between the ionization rate measured in diffuse and dense interstellar clouds. We collect the most recent experimental and theoretical data on the cross sections for the production of H2+ and He+ by electron and proton impact, and we discuss the available constraints on the cosmic-ray fluxes in the local interstellar medium. Starting from different extrapolations at low energies of the demodulated cosmic-ray proton and electron spectra, we compute the propagated spectra in molecular clouds in the continuous slowing-down approximation taking into account all the relevant energy loss processes. The theoretical value of the cosmic-ray ionization rate as a function of the column density of traversed matter is in agreement with the observational data only if either the flux of cosmic-ray electrons or of protons increases at low energies. The most successful models are characterized by a significant (or even dominant) contribution of the electron component to the ionization rate, in agreement with previous suggestions. However, the large spread of cosmic-ray ionization rates inferred from chemical models of molecular cloud cores remains to be explained. Available data combined with simple propagation models support the existence of a low-energy component (below about 100 MeV) of cosmic-ray electrons or protons responsible for the ionization of molecular cloud cores and dense protostellar envelopes.