Face on Surface Brightness Profile For Spiral Galaxies

In summary, the exponential decrease in surface brightness of spiral galaxies is due to the inside-out formation of the galaxy's disk and the conservation of angular momentum of the gas clouds during star formation.
  • #1
blumfeld0
148
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Why does the face on surface brightness profile of spiral galaxies follow an exponential decrease with incresing distance from the center? Why is it exponential as opposed to linear or some power law? seems like 'e' shows up a lot.

I know it is an obervational fact that they exhibit this behavior (it's also been confirmed in numerical simulations) but does anyone know what the mechanism involved here is? I don't know maybe I am asking too deep a question here but I really am curious as to a known explanation.
Is it related to conservation of angular momentum when sprials form maybe?blumfeld0
 
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  • #2
's answerThe exponential decrease in surface brightness can be explained by the inside-out formation of a galaxy's disk. When the galaxy forms, it begins to form stars at the center first and then slowly moves out in radius as the galaxy's gravitational potential weakens. This is because the gas clouds, which form stars, are able to collapse more easily when the gravity is stronger near the center, allowing for an increased star formation rate. This mechanism explains why the star formation rate decreases with increasing distance from the center, resulting in an exponential decrease in the surface brightness of the galaxy. The exponential decrease is also due to the conservation of angular momentum of the gas clouds. As the gas clouds collapse to form stars, they conserve their angular momentum, preventing them from collapsing too quickly and instead spreading out in a disk. This results in the exponential decrease in surface brightness as the stars are spread out over a larger area.
 

1. What is a face on surface brightness profile for spiral galaxies?

A face on surface brightness profile for spiral galaxies is a graph that shows the brightness of a spiral galaxy as seen from a direct, face-on view. It is a way to visualize the distribution of stars and gas within the galaxy, with the center of the galaxy being the brightest point on the graph.

2. How is a face on surface brightness profile created?

A face on surface brightness profile is created by measuring the brightness of a spiral galaxy at different distances from its center, and plotting these measurements on a graph. This is typically done using images taken by telescopes, which can capture the light emitted by stars and gas in the galaxy.

3. What information can we learn from a face on surface brightness profile?

A face on surface brightness profile can provide information about the structure and composition of a spiral galaxy. It can reveal the presence of spiral arms, bulges, and other features, as well as the distribution of stars and gas within the galaxy. It can also be used to estimate the total mass and luminosity of the galaxy.

4. How does the shape of a face on surface brightness profile vary among different spiral galaxies?

The shape of a face on surface brightness profile can vary greatly among different spiral galaxies. Some may have a smooth and gradual decline in brightness from the center to the outer edges, while others may have distinct peaks and valleys. This variation depends on factors such as the size, age, and formation history of the galaxy.

5. What can a face on surface brightness profile tell us about the evolution of spiral galaxies?

By studying the face on surface brightness profiles of different spiral galaxies, scientists can gain insight into the evolution of these galaxies over time. For example, the presence of a bulge in the profile can suggest that a galaxy has undergone a merger with another galaxy. Changes in the shape and brightness of the profile can also reveal how the galaxy has grown and evolved over time.

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