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1 Ch 14: Our Milky Way Meet our own galaxy big, spiralarmed and full of surprises.

2 Meet the Milky Way Now, we move up to the next level: a galaxy made up of A core dense with stars. Billions of stars in the spiral arms. Star clusters in the halo. In between is gas and vacuum.

3 Milky Way to the Ancients To ancient peoples, the Milky Way was just that: Greeks milk flowing from Mount Olympus Native Americans river of light that nourished the constellation animals Mid-Eastern river of nourishment from God.

4 What Does It Look Like Today? Even in my backyard, the Milky Way shows up as a band of light running across the sky, but looks like this wide angle picture. The light clouds are stars in our own and other spiral arms of the galaxy. The dark clouds are dust clouds in our arm of the galaxy that block our view of the rest of the Milky Way.

5 Where are We? Our best understanding today is that we are: In the outer part of one of the spiral arms. About t 28,000 LY out from the nucleus of the galaxy. In the galactic disk. In among stars that are young and metalrich (part of the rebirth after supernovas).

6 What is the rest of the galaxy like? Our understanding of the rest of the galaxy mostly depends on our ability to see it. We know we are on one of four spiral arms Most of the stars we see are only in our spiral arm. The galactic nucleus is incredibly bright and dusty, so we can t see what is going g on, except by x-rays and radio wave observations. Dust clouds in our spiral arm and in inner arms partially block our view of the sky beyond our galaxy.

7 A Sea of Stars Our galaxy is made up of spiral arms filled with billions of stars and surrounding the whole galaxy is a halo of globular clusters of stars (two globular clusters at right). Around the core, there is a thicker distribution of stars in the nuclear bulge a sort of flattened out sphere that trails and thins down into the galactic disk.

8 Where are the Globular Clusters? Using RR Lyrae variable stars and Leavitt s work, Shapely measured the distance to various globular l clusters. He discovered that in He discovered that in a 3D layout, there was a uniform halo of clusters centered around the core, not the Earth!

9 What Makes Up The Rest? What is there between the stars? Light gases. This gas is the interstellar medium it is very thin and mostly made up of hydrogen gas. There are some more complex molecules like water (H20) and carbon monoxide (CO) There really aren t any dust grains or stray asteroids or comets floating out there.

10 Where does the gas come from? The figure at left shows the source of the interstellar medium supernova! Supernova explode and release their gases. These gases expand and form very thin clouds. Someday, another supernova s explosion will compress this cloud and new stars will form.

11 How common are supernova? Supernova are not terribly common, but then space is also terribly vast. On average we observe several hundred supernova in the Milky Way per year from Earth. So, over the course of 1 billion years, the odds are that t there will be a supernova within 5 LY of any point that may be enough hto compress a cloud.

12 Where is the gas now? The gas is everywhere throughout the galaxy. We can t see most of it because it is soooo cold (near absolute zero) and not radiating any light or heat. It is concentrated around stars, but not too close The heat of star formation creates a halo of gases, much like the Kuiper belt of comets.

13 Radio Views of the Galaxy Based on recent radio observations of the galaxy, this is the distribution of H II in the galaxy as seen from above the galactic poles: Definitely spiral arms Core shields our view of the other side of the galaxy and makes the dark wedge. These H II emissions are linked to stars and protostar formation.

14 Compared to Another Spiral Galaxy This is the visible and radio views of another spiral galaxy, M83. Notice how hydrogen gas emissions in the radio view are linked with blue gaseous regions in the spiral arms where stars are forming. Good confirmation of our radio view of the Milky Way.

15 Other Details of Us Also, our view of M83 shows bright red H II regions in the outer arms These are extremely bright regions of star birth. We can also see a supernova (lower right).

16 Our best idea of what the Milky Way looks like

17 What Does the Core Look Like? Based on radio and x- ray observations, we think that there are two possible shapes of the Milky Way s core: Left: the classic Spiral Right: the barred spiral.

18 The Milky Way Seen From Far Away

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