Shocks and Molecules in Diffuse Interstellar Cloud Pairs

TL;DR

This study combines observations and MHD shock models to analyze shock fronts in diffuse interstellar cloud pairs, revealing how shocks influence cloud morphology, kinematics, and molecular cloud formation.

Contribution

It introduces a detailed comparison of MHD shock models with multi-wavelength observations of high-latitude clouds, highlighting the role of shocks and magnetic fields in cloud evolution.

Findings

High-velocity HI gas indicates active shocks at cloud edges.

Cloud morphology shows arcs consistent with shock fronts.

Simulations replicate observed features, suggesting magnetic alignment influences cloud structure.

Abstract

The diffuse interstellar medium is dynamic, and its chemistry and evolution is determined by shock fronts as well as photodissociation. Shocks are implied by the supersonic motions and velocity dispersion often statistically called "turbulence". We compare models of magnetohydrodynamic (MHD) shocks, with speeds typical of cloud motions through the ISM (3-25 km/s) and densities typical of cold neutral gas (~ 100 cm-3), to archival observations of the atomic hydrogen 21-cm line for gas kinematics, far-infrared emission for dust mass, and mid-infrared emission for high-resolution morphology, to identify shock fronts in three high-latitude clouds pairs with masses of order 50 suns. The clouds have `heads' with extended `tails', and high-resolution images show arcs on the leading edges of the "heads" that could be individual shocks. The HI shows higher-velocity gas at the leading edges due to shock-accelerated material. For two cloud pairs, one cloud has an active shock indicated by broad and offset HI, while the other cloud has already been shocked and is predominantly `CO-dark' molecular hydrogen. Two-dimensional MHD simulations for shocks parallel to the magnetic field for pairs of clouds show a remarkable similarity to observed cloud features, including merged "tails" due to aligned flow and magnetic field, which leads to lateral confinement downstream. A parallel alignment between magnetic field and gas flow may lead to formation of small molecular clouds.