THE INTERSTELLAR MEDIUM
Properties of neutral and ionized interstellar gas, giant molecular clouds, the warm and hot intercloud medium, supernova remnants, and interstellar dust. Physical processes in low density gases including radiation transfer, excitation and ionization of interstellar atoms and molecules, and the interaction between gas and dust.
Prerequisites & course information
Requisites: ASTRON 200 and ( PHYSICS 241 , 249 , PHYSICS/E C E 235 , or concurrent enrollment) Course Designation: Core GenEd - Natural Science & Wellness Breadth - Physical Science Level - Advanced L&S Credit - L&S Liberal Arts and Science Repeatable for Credit: No Last Taught: Fall 2025 Learning Outcomes: 1. Describe characteristics of various phases of the interstellar medium (ISM) and explain why these particular phases are stable. Audience: Undergraduate 2. Explain key physical processes in each phase of ISM. Audience: Undergraduate 3. For a given set of observations of spectral lines, derive basic physical properties, such as temperature, density, and the total column density of the species. Audience: Undergraduate 4. Analyze the effects and roles of dust in the ISM. Audience: Undergraduate 5. For a given set of initial physical conditions, compose equations to describe the environment, and apply these equations to predict the excitation and ionization conditions, molecular abundances, temperatures, and densities of the ISM environment. Audience: Undergraduate 6. Explain current theories on how stars and planets form to family and friends. Audience: Undergraduate Learning Outcomes: 1. Describe characteristics of various phases of the interstellar medium (ISM) and explain why these particular phases are stable. Audience: Undergraduate 2. Explain key physical processes in each phase of ISM. Audience: Undergraduate 3. For a given set of observations of spectral lines, derive basic physical properties, such as temperature, density, and the total column density of the species. Audience: Undergraduate 4. Analyze the effects and roles of dust in the ISM. Audience: Undergraduate 5. For a given set of initial physical conditions, compose equations to describe the environment, and apply these equations to predict the excitation and ionization conditions, molecular abundances, temperatures, and densities of the ISM environment. Audience: Undergraduate 6. Explain current theories on how stars and planets form to family and friends. Audience: Undergraduate
Sources
- Course catalogue ↗2026-2027