14.2 Galactic Recycling Our Goals for Learning • How does our galaxy recycle gas into stars? • Where do stars tend to form in our galaxy?

How does our galaxy recycle gas into stars?

Star-gas-star cycle Recycles gas from old stars into new star systems

High-mass stars have strong stellar winds that blow bubbles of hot gas

Lower mass stars return gas to interstellar space through stellar winds and planetary nebulae

X-rays from hot gas in supernova remnants reveal newly-made heavy elements

Supernova remnant cools and begins to emit visible light as it expands New elements made by supernova mix into interstellar medium

Multiple supernovae create huge hot bubbles that can blow out of disk; gas cooling in the halo can rain back down on disk.

Atomic hydrogen gas forms as hot gas cools, allowing electrons to join with protons. Molecular clouds form next, after gas cools enough to allow to atoms to combine into molecules

Molecular clouds in Orion Composition: Mostly H2 About 28% He About 1% CO Many other molecules

Gravity forms stars out of the gas in molecular clouds, completing the star-gas-star cycle

Radiation from newly formed stars is eroding these star-forming clouds

Summary of Galactic Recycling Stars make new elements by fusion Dying stars expel gas and new elements, producing hot bubbles (~106 K) Hot gas cools, allowing atomic hydrogen clouds to form (~100-10,000 K) Further cooling permits molecules to form, making molecular clouds (~30 K) Gravity forms new stars (and planets) in molecular clouds Gas Cools

Where will most of the mass now in our galaxy’s gas be in a hundred billion years? Blown out of the galaxy Still recycling just like it is now Locked into white dwarfs and low-mass stars :00

We observe star-gas-star cycle operating in Milky Way’s disk using many different wavelengths of light

Infrared Visible Infrared light reveals stars whose visible light is blocked by gas clouds

X-rays X-rays are observed from hot gas above and below the Milky Way’s disk

Radio (21cm) 21-cm radio waves emitted by atomic hydrogen show where gas has cooled and settled into disk

Radio (CO) Radio waves from carbon monoxide (CO) show locations of molecular clouds

IR (dust) Long-wavelength infrared emission shows where young stars are heating dust grains

Gamma rays show where cosmic rays from supernovae collide with atomic nuclei in gas clouds

Where do stars tend to form in our galaxy?

Ionization nebulae are found around short-lived high-mass stars, signifying active star formation Orion nebula

Reflection nebulae scatter the light from stars. Why do reflection nebulae look blue, even when the stars near them aren't blue? Chamaeleon 1 complex (VLT UT1+FORS1) V, R, and I bands http://www.eso.org/outreach/gallery/vlt/images/Top20/Top20/top8.html

Reflection nebulae scatter the light from stars Why do reflection nebulae look bluer than the nearby stars? For the same reason that our sky is blue! Chamaeleon 1 complex (VLT UT1+FORS1) V, R, and I bands http://www.eso.org/outreach/gallery/vlt/images/Top20/Top20/top8.html

What kinds of nebulae do you see?

Halo: No ionization nebulae, no blue stars  no star formation Disk: Ionization nebulae, blue stars  star formation

Much of star formation in disk happens in spiral arms Whirlpool Galaxy

Much of star formation in disk happens in spiral arms Ionization Nebulae Blue Stars Gas Clouds Whirlpool Galaxy

Spiral arms are waves of star formation

Spiral arms are waves of star formation Gas clouds get squeezed as they move into spiral arms Squeezing of clouds triggers star formation Young stars flow out of spiral arms

What have we learned? • How does our galaxy recycle gas into stars? Stacie Kent: Insert thumbnail of 14.8 What have we learned? • How does our galaxy recycle gas into stars? Stars are born from the gravitational collapse of gas clumps in molecular clouds. Near the ends of their lives, stars more massive than our Sun create elements heavier than hydrogen and helium and expel them into space via supernovae and stellar winds. The supernovae and winds create hot bubbles in the interstellar medium, but the gas within these bubbles gradually slows and cools as they expand. Eventually, this gas cools enough to collect into clouds of atomic hydrogen. Further cooling allows atoms of hydrogen and other elements to collect into molecules, producing molecular clouds.These molecular clouds then form stars, completing the star–gas–star cycle.

What have we learned? • Where do stars tend to form in our galaxy? Active star-forming regions, marked by the presence of hot, massive stars and ionization nebulae, are found preferentially in spiral arms. The spiral arms represent regions where a spiral density wave has caused gas clouds to crash into each other, thereby compressing them and making star formation more likely.

Activity 19, pages 67-70

1B: The hotter a star’s temperature, the ____ the wavelength at which its peak emission occurs. Smaller Larger (stays the same) :00

1C: A star whose spectrum peaks at 300 nm is ___ than the stars in Fig Hotter Cooler It depends; need more info :00

2. Who’s right? Felix Isidor Neither Both :00

3D: Two stars are of equal size. Which radiates more ultraviolet energy? T=5000 K star T=8000 K star Both radiate the same It depends; more info needed :00

3E: If two visible stars are identical in distance and size, the hotter one will appear to be the ____ of the two in the night sky. Brighter Dimmer It depends; need more info :00

6A: Which of the 3 stars in Figure 2 is the hottest? B C :00

6B: Which star is coolest? :00

6C: Which star is most luminous? B C :00

6D:Which is larger, star A or star B? Same size More info needed :00

6E: Which star(s) will appear red? B C None of them All of them :00