1. Note that the following lectures include animations and PowerPoint effects such as fly-ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode).

2. The Interstellar Medium Chapter 10

3. You have begun your study of the sun and other stars, but now it is time to focus on the thin gas and dust that drifts through space between the stars. This chapter will show you how important this material is to the story of stars and will help you answer three important questions: How do astronomers study the gas and dust between the stars, called interstellar medium? What kinds of material make up the interstellar medium? How does the interstellar medium interact with the stars? The gas and dust between the stars is the starting point for the life story of the stars. The next four chapters will trace the birth, life, and death of stars. Guidepost

4. I. Studying the Interstellar Medium A. Nebulae B. Extinction and Reddening C. Interstellar Absorption Lines D. Interstellar Emission Lines E. Infrared Radiation from Dust II. Components of the Interstellar Medium A. Cool Clouds B. The Intercloud Medium C. Molecular Clouds D. Coronal Gas III. The Gas-Stars-Gas Cycle A. Gas and Dust from Aging Stars B. A Preview of Star Formation Outline

5. A World of Dust We are interested in the interstellar medium because… a) dense interstellar clouds are the birth place of stars b) Dark clouds alter and absorb the light from stars behind them The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky.

6. Bare-Eye Nebula: Orion One example of an interstellar gas cloud (nebula) is visible to the bare eye: the Orion nebula

7. Three Kinds of Nebulae (1) 1) Emission Nebulae Hot star illuminates a gas cloud; excites and/or ionizes the gas (electrons kicked into higher energy states); electrons recombining, falling back to ground state produce emission lines The Fox Fur Nebula NGC 2246 The Trifid Nebula

8. Three Kinds of Nebulae (2) Star illuminates a gas and dust cloud; star light is reflected by the dust; reflection nebulae appear blue because blue light is scattered by larger angles than red light; the same phenomenon makes the day sky appear blue (if it’s not cloudy) 2) Reflection Nebulae

9. Three Kinds of Nebulae (3) Dense clouds of gas and dust absorb the light from the stars behind; Barnard 86 Horsehead Nebula appear dark in front of the brighter background; 3) Dark Nebulae

10. Red light can more easily penetrate the cloud, but is still absorbed to some extent. Interstellar Reddening Blue light is strongly scattered and absorbed by interstellar clouds. Infrared radiation is hardly absorbed at all. Interstellar clouds make background stars appear redder. Visible Barnard 68 Infrared

11. Interstellar Reddening (2) The Interstellar Medium absorbs light more strongly at shorter wavelengths.

12. Interstellar Reddening (3) Nebulae that appear as dark nebulae in the optical, can shine brightly in the infrared due to blackbody radiation from the warm dust.

13. Interstellar Absorption Lines The interstellar medium produces absorption lines in the spectra of stars. These can be distinguished from stellar absorption lines through: a) Absorption from wrong ionization states Narrow absorption lines from Ca II: Too low ionization state and too narrow for the O star in the background; multiple components b) Small line width (too low temperature; too low density) c) Multiple components (several clouds of ISM with different radial velocities)

14. Observing Neutral Hydrogen: The 21-cm (radio) line (I) Electrons in the ground state of neutral hydrogen have slightly different energies, depending on their spin orientation. Magnetic field due to proton spin Magnetic field due to electron spin Opposite magnetic fields attract => Lower energy Equal magnetic fields repel => Higher energy 21 cm line

15. The 21-cm Line of Neutral Hydrogen (II) Transitions from the higher-energy to the lower- energy spin state produce a characteristic 21-cm radio emission line. => Neutral hydrogen (HI) can be traced by observing this radio emission.

16. Observations of the 21-cm Line (1) All-sky map of emission in the 21-cm line G a l a c t i c p l a n e

17. Observations of the 21-cm Line (2) HI clouds moving towards Earth (from redshift/blueshift of line) HI clouds moving away from Earth Individual HI clouds with different radial velocities resolved

18. Interstellar Dust Probably formed in the atmospheres of cool stars Mostly observable through infrared emission Spitzer Space Telescope (infrared) image of interstellar dust near the center of our Milky Way (Right:) Infrared Emission from interstellar dust and gas molecules in the “Whirlpool Galaxy” M51

19. Structure of the ISM HI clouds: Hot intercloud medium: The ISM occurs in two main types of clouds: Cold (T ~ 100 K) clouds of neutral hydrogen (HI); moderate density (n ~ 10 – a few hundred atoms/cm 3 ); size: ~ 100 pc Hot (T ~ a few 1000 K), ionized hydrogen (HII); low density (n ~ 0.1 atom/cm 3 ); gas can remain ionized because of very low density

20. Molecules in Space In addition to atoms and ions, the interstellar medium also contains molecules. Molecules also store specific energies in their a) rotation b) vibration Transitions between different rotational / vibrational energy levels lead to emission – typically at radio wavelengths

21. The Most Easily Observed Molecules in Space CO = Carbon Monoxide  Radio emission OH = Hydroxyl  Radio emission The Most Common Molecule in Space: Difficult to observe! Use CO as a tracer for H 2 in the ISM! H 2 = Molecular Hydrogen  Ultraviolet absorption and emission: But: Where there’s H 2, there’s also CO

22. Molecular Clouds Molecules are easily destroyed (“dissociated”) by ultraviolet photons from hot stars.  They can only survive within dense, dusty clouds, where UV radiation is completely absorbed.  “Molecular Clouds”: Largest molecular clouds are called “Giant Molecular Clouds”: Diameter ≈ 15 – 60 pc Temperature ≈ 10 K Total mass ≈ 100 – 1 million solar masses Cold, dense molecular cloud core HI Cloud UV emission from nearby stars destroys molecules in the outer parts of the cloud; is absorbed there. Molecules survive

23. Molecular Clouds (2) The dense cores of Giant Molecular Clouds are the birth places of stars.

24. The Coronal Gas Additional component of very hot, low-density gas in the ISM: n ~ 0.001 particles/cm 3 Observable in X-rays Called “Coronal gas” because of its properties similar to the solar corona (but completely different origin!) Probably originates in supernova explosions and winds from hot stars Our sun is located within (near the edge of) a coronal gas bubble. T ~ 1 million K

25. The Four Components of the Interstellar Medium

26. The Gas-Star-Gas Cycle All stars are constantly blowing gas out into space (recall: Solar wind!) The more luminous the star is, the stronger is its stellar wind. These winds are particularly strong in aging red giant stars.

27. The Gas-Stars-Gas Cycle Stars, gas, and dust are in constant interaction with each other.