# Two-photon production in low-velocity shocks

## TL;DR

This paper investigates the emission processes of low-velocity shocks in the interstellar medium, emphasizing the role of the two-photon continuum as a key FUV tracer, and provides practical formulas for modeling their radiative yields.

## Contribution

It introduces new fitting formulas for the emission yields of Ly-alpha, two-photon continuum, and H-alpha in hydrogen plasma, aiding modeling of low-velocity shock cooling.

## Key findings

- FUV band is an effective tracer of low-velocity shocks.
- GALEX FUV images reveal large interstellar structures and bow shocks.
- Provided formulas facilitate incorporation into cooling and ionization models.

## Abstract

The Galactic interstellar medium abounds in low-velocity shocks with velocities less than, say, about 70 km/s. Some are descendants of higher velocity shocks, while others start off at low velocity (e.g., stellar bow shocks, intermediate velocity clouds, spiral density waves). Low-velocity shocks cool primarily via Ly-alpha, two-photon continuum, optical recombination lines (e.g., H-alpha), free-bound emission, free-free emission and forbidden lines of metals. The dark far-ultraviolet (FUV) sky, aided by the fact that the two-photon continuum peaks at 1400 angstroms, makes the FUV band an ideal tracer of low-velocity shocks. Recent GALEX FUV images reaffirm this expectation, discovering faint and large interstellar structure in old supernova remnants and thin arcs stretching across the sky. Interstellar bow shocks are expected from fast stars from the Galactic disk passing through the numerous gas clouds in the local interstellar medium within 15 pc of the Sun. Using the best atomic data available to date, we present convenient fitting formulae for yields of Ly$\alpha$, two-photon continuum and H$\alpha$ for pure hydrogen plasma in the temperature range of 10^4 K to 10^5 K. The formulae presented here can be readily incorporated into time-dependent cooling models as well as collisional ionization equilibrium models.