— Ch. 1 · Defining The Interstellar Medium —
Interstellar medium.
~5 min read · Ch. 1 of 7
The space between stars is not empty. It holds matter and radiation that astronomers call the interstellar medium. This substance includes gas in ionic, atomic, and molecular forms alongside dust and cosmic rays. It fills the vast distances between star systems within a galaxy. The density of atoms here remains far below even the best laboratory vacuums on Earth. Yet collisions occur frequently enough over short distances to make it behave like a gas or plasma. Electromagnetic radiation interacts with this material rather than passing through unaffected particles. Hydrogen dominates the composition followed by helium with trace amounts of carbon oxygen and nitrogen. By mass ninety-nine percent of the interstellar medium consists of gas while one percent comprises dust grains.
Phases And Thermal Equilibrium
Matter exists in multiple phases distinguished by ionization state temperature and density. A static two-phase model once explained these properties with cold dense clouds and warm intercloud regions. Later research added a dynamic third phase representing very hot gas shock-heated by supernovae. These phases reach temperatures where heating and cooling achieve stable equilibrium. Hot regions generally possess low particle number densities because pressure balance requires expansion. Coronal gas maintains high temperatures for hundreds of millions of years due to rare particle collisions. Once temperatures fall to around one hundred thousand Kelvin protons recombine with electrons to form hydrogen atoms. This process emits photons that carry energy away leading to runaway cooling. OB stars produce photons energetic enough to ionize neutral hydrogen creating a dynamic equilibrium between ionization and recombination. The boundary between warm ionized and warm neutral media marks where all ionizing photons are consumed.