Supernova enhanced cosmic ray ionization and induced chemistry in a molecular cloud of W51C

TL;DR

This study presents evidence that a molecular cloud near the W51C supernova remnant experiences significantly enhanced cosmic ray ionization, leading to distinct high- and low-ionization phases in its chemistry, driven by freshly accelerated cosmic rays.

Contribution

It provides observational evidence of elevated cosmic ray ionization rates and the coexistence of high- and low-ionization phases in a molecular cloud influenced by a supernova remnant.

Findings

Ionization rate ~10^-15 s^-1, 100 times higher than typical.

High electron fraction (~10^-5) in large cloud regions.

Simultaneous presence of high- and low-ionization phases (HIP and LIP).

Abstract

Cosmic rays pervade the Galaxy and are thought to be accelerated in supernova shocks. The interaction of cosmic rays with dense interstellar matter has two important effects: 1) high energy (>1 GeV) protons produce {\gamma}-rays by {\pi}0-meson decay; 2) low energy (< 1 GeV) cosmic rays (protons and electrons) ionize the gas. We present here new observations towards a molecular cloud close to the W51C supernova remnant and associated with a recently discovered TeV {\gamma}-ray source. Our observations show that the cloud ionization degree is highly enhanced, implying a cosmic ray ionization rate ~ 10-15 s-1, i.e. 100 times larger than the standard value in molecular clouds. This is consistent with the idea that the cloud is irradiated by an enhanced flux of freshly accelerated low-energy cosmic rays. In addition, the observed high cosmic ray ionization rate leads to an instability in the chemistry of the cloud, which keeps the electron fraction high, ~ 10-5, in a large fraction (Av \geq 6mag) of the cloud and low, ~ 10-7, in the interior. The two states have been predicted in the literature as high- and low-ionization phases (HIP and LIP). This is the observational evidence of their simultaneous presence in a cloud.