The Distribution of Thermal Pressures in the Interstellar Medium

TL;DR

This paper investigates the distribution of thermal pressures in the interstellar medium using UV absorption spectra, revealing most gas at moderate pressures but also widespread high-pressure regions likely caused by turbulent density enhancements.

Contribution

It provides the first detailed distribution function of thermal pressures in H I regions based on high-resolution UV spectra from Hubble, highlighting the prevalence of high-pressure gas.

Findings

Most interstellar gas has thermal pressures between 1000 and 10,000 cm^{-3}K.

Evidence of high-pressure gas exceeding 10^5 cm^{-3}K is widespread but constitutes a small fraction.

High-pressure regions are likely caused by small-scale, short-lived density enhancements from turbulent flows.

Abstract

It is generally recognized that the interstellar medium has a vast range of densities and temperatures. While these two properties are usually anticorrelated with each other, there are nevertheless variations in their product, i.e., the thermal gas pressure divided by the Boltzmann constant k. In neutral gas, the relative populations of neutral carbon atoms in the excited fine-structure states can give a direct measure of a local thermal pressure. A picture of the distribution function for thermal pressures in H I regions is now arising from a survey of interstellar C I absorption features in the UV spectra of 21 early-type stars, observed with a wavelength resolving power of 200,000 by the STIS instrument on the Hubble Space Telescope. Most of the gas is within the range 1000 < p/k < 10,000 cm^{-3}K, but there is also evidence for some of the material being at much higher pressures, i.e., p/k > 10^5 cm^{-3}K. While the fraction of gas at these elevated pressures is quite small, it seems nearly ubiquitous. This phenomenon may arise from small-scale, short-lived density enhancements that are produced by converging flows of material in supersonic turbulence.