Back To CourseBasics of Astronomy
28 chapters | 325 lessons
As a member, you'll also get unlimited access to over 70,000 lessons in math, English, science, history, and more. Plus, get practice tests, quizzes, and personalized coaching to help you succeed.Free 5-day trial
As you look at an artist's conception of how the Milky Way galaxy looks from afar, the coolest feature has got to be those funky-looking spiral arms. Spiral arms are concentrations of gas and dust extending from the center of a galaxy in a pinwheel shape.
Note a couple of things. I mentioned the image is an artist's conception, and I mentioned the spiral arms contain dust. Clearly, there are two problems. First, we can't see the actual shape of our galaxy because we are inside of it, and second, plenty of what we can see is obstructed from view by the dust in the interstellar medium.
This should naturally make you wonder how we even know our galaxy has spiral arms to begin with. Stick around, because this lesson will explain how we know this to be the case.
The answer lies in radio waves, a type of electromagnetic radiation, with long wavelengths, which can penetrate the interstellar medium.
We know that hydrogen is the most abundant element in our universe and that hydrogen atoms will emit visible light if their electrons are excited. So, to figure out how matter is spread around our galaxy, we need to look for concentrations of hydrogen gas. Unfortunately, the excitation of hydrogen is not likely to occur in the cold reaches of interstellar space, and thus, we are unable to see concentrations of hydrogen with ordinary light telescopes.
I mean, it's hard to get excited, energized, and move around when you're really cold. You sort of freeze up in cold weather. Hydrogen atoms act the same way out in the cold depths of space.
Even if hydrogen were to be excited, the visible light emitted as a consequence of this excitation would be blocked by the interstellar dust. Again, that would render our ordinary telescopes basically useless for this endeavor. The interstellar dust is basically like a really thick cloud. Like a thick cloud blocks out the light of the sun, a thick interstellar cloud of dust and gas would block any glowing hydrogen atoms.
Yet we have a trick up our sleeves when it comes to mapping out the distribution of hydrogen in our galaxy; it is the radio waves I defined before. This is because even the cold hydrogen clouds, containing neutral hydrogen, or H I Hydrogen, will emit radio waves. Another way to think of H I hydrogen is as unexcited hydrogen.
So how do radio telescopes actually tell us that spiral arms exist in our galactic disk? Astronomers can use the Doppler effect to help map out the hydrogen in our galaxy. The Doppler effect, or Doppler shift, is an apparent change in the frequency of a wave caused by the motion of the observer or source emitting the wave. I encourage you to watch the lesson describing it for more detail.
But to avoid confusion, I'm going to boil everything down to this. Different Doppler shifts throughout our galaxy cause radio waves hitting our radio telescopes to arrive with different wavelengths. This allows us to sort and visualize the gas clouds in our galaxy using a map of neutral hydrogen.
The image on your screen clearly shows you that neutral hydrogen is not spread uniformly in our galaxy's disk, but rather in lanes of sorts that look like arches and spirals that have branches, gaps, and spurs. We see similar features in other spiral galaxies.
Additionally, these same spiral galaxies have spiral arms that are outlined by very hot, luminous stars. The patterns of spiral arms mapped out by neutral hydrogen and visible light coming from these galaxies are basically the same. This indicates to us that our galaxy's map of neutral hydrogen is representative of our galaxy's spiral arms that are outlined to observers from afar by very bright stars.
But don't be fooled! Stars are distributed pretty evenly throughout the disk of a galaxy. The reason the spiral arms stand out so much is because, like I said before, it's where the hottest and most luminous stars are found. That gives the spiral arms a big glow out in space compared to the rest of the disk!
Spiral arms are concentrations of gas and dust extending from the center of a galaxy in a pinwheel shape. We can't see our own spiral arms with light telescopes from afar. But we can see that other spiral galaxies have arms that glow out in space due to the hot and luminous stars within them. The patterns of light created by these stars, resembling spirals, match up to the patterns created by the map of such a galaxy's neutral hydrogen, or H I Hydrogen, which emits radio waves.
Radio waves are a type of electromagnetic radiation, with long wavelengths, which can penetrate the interstellar medium, and therefore, help us map out our own galaxy's concentrations of hydrogen gas. Just such a map of neutral hydrogen clearly shows arches and spirals of neutral hydrogen. This implies such areas contain hot, luminous stars in our own galaxy, giving it glowing spiral arms when viewed from afar.
By the end of this lesson, you should be able to:
To unlock this lesson you must be a Study.com Member.
Create your account
Did you know… We have over 95 college courses that prepare you to earn credit by exam that is accepted by over 2,000 colleges and universities. You can test out of the first two years of college and save thousands off your degree. Anyone can earn credit-by-exam regardless of age or education level.
To learn more, visit our Earning Credit Page
Not sure what college you want to attend yet? Study.com has thousands of articles about every imaginable degree, area of study and career path that can help you find the school that's right for you.
Back To CourseBasics of Astronomy
28 chapters | 325 lessons