<p>In terms of the distribution of stellar masses <em>when stars form</em> -- the <a href="https://en.wikipedia.org/wiki/Initial_mass_function" rel="nofollow noreferrer">Initial Mass Function</a> (IMF) -- there doesn't seem to be much variation, at least for spirals. (There is evidence that massive elliptical galaxies may have different IMFs as a function of radius, with relatively more <em>low-mass</em> stars formed near their centers. The cause of this is unclear; it might have to do with different conditions for star formation, with very dense, high-pressure gas in what would become the centers of massive elliptical galaxies possibly producing different distributions of stellar masses.)</p>

<p>The <em>current</em> distribution of stellar masses at a given radius in a spiral galaxy will depend almost entirely on the local star-formation history. Since stellar lifetime depends on stellar mass, regions with recent star formation will have more stars that are massive; regions where star formation ceased a long time ago will be dominated by low-mass stars, since all the higher-mass stars there have died.</p>

<p>In most spiral galaxies, the mean age of stars tends to decrease as you move further out in radius (as indicated by optical colors: reddish central regions are mostly old populations dominated by red giants, while the disk further out is blue because there are younger populations dominated by hot, massive stars). This is an example of what's called "inside-out" star formation.</p>

<p>However, a lot of lower-mass spirals seem to show a reversal of this trend at large radii, with redder (older, mostly lower-mass) stars beyond a certain radius. Since this is the same radius at which the density of stars in the disk stars falling off more rapidly (the "break" or "truncation" radius), it's usually thought this is the result of a combination of two effects: 1) A radial threshold/cutoff in star formation, with very few stars being formed beyond a certain radius (possibly because the gas density becomes too low); and 2) Radial scattering of stars over time by spiral arms, which means that older stars tend to be scattered to larger (or smaller) radii simply because they've had more encounters with spiral arms. In this case, the relative fraction of more massive stars would <em>increase</em> with radius out to the truncation radius, and then decrease beyond.</p>

CC BY-SA 4.0
2020-05-24T10:30:16.507Z
2020-05-24T10:30:16.507Z
Peter Erwin
<p>As we move away from the centre of, say, a spiral galaxy, is there a relation between the stellar mass and distance?
I know the how the stellar <s>abundance</s> number and density varies with the distance but does stellar mass also follow a pattern?</p>

CC BY-SA 4.0
2019-12-24T08:54:30.843Z
All of these are areas of active research. Incidentally, what do you mean by "stellar abundance"? If you mean how does the chemical composition of stars vary with radius, then that is quite complex and likely age dependent.
ProfRob
CC BY-SA 4.0
2019-12-24T15:30:45.570Z
No, I do not mean chemical composition. I was simply referring to the number density of stars when I said “stellar abundance”
Khurana
<star><galaxy>
Correlation between stellar mass and galactocentric distance
Khurana
# Correlation between stellar mass and galactocentric distance

(Asked by: username_0 on 2019-12-24)

As we move away from the centre of, say, a spiral galaxy, is there a relation between the stellar mass and distance?
I know the how the stellar ~~abundance~~ number and density varies with the distance but does stellar mass also follow a pattern?

**Tags:** star, galaxy
> **Comments:**
> **username_1**: All of these are areas of active research. Incidentally, what do you mean by "stellar abundance"? If you mean how does the chemical composition of stars vary with radius, then that is quite complex and likely age dependent.  
> **username_0**: No, I do not mean chemical composition. I was simply referring to the number density of stars when I said “stellar abundance”  

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## 1 answers

### Answer by username_2 on 2020-05-24. Score: 4

In terms of the distribution of stellar masses *when stars form* -- the [Initial Mass Function](https://en.wikipedia.org/wiki/Initial_mass_function) (IMF) -- there doesn't seem to be much variation, at least for spirals. (There is evidence that massive elliptical galaxies may have different IMFs as a function of radius, with relatively more *low-mass* stars formed near their centers. The cause of this is unclear; it might have to do with different conditions for star formation, with very dense, high-pressure gas in what would become the centers of massive elliptical galaxies possibly producing different distributions of stellar masses.)

The *current* distribution of stellar masses at a given radius in a spiral galaxy will depend almost entirely on the local star-formation history. Since stellar lifetime depends on stellar mass, regions with recent star formation will have more stars that are massive; regions where star formation ceased a long time ago will be dominated by low-mass stars, since all the higher-mass stars there have died.

In most spiral galaxies, the mean age of stars tends to decrease as you move further out in radius (as indicated by optical colors: reddish central regions are mostly old populations dominated by red giants, while the disk further out is blue because there are younger populations dominated by hot, massive stars). This is an example of what's called "inside-out" star formation.

However, a lot of lower-mass spirals seem to show a reversal of this trend at large radii, with redder (older, mostly lower-mass) stars beyond a certain radius. Since this is the same radius at which the density of stars in the disk stars falling off more rapidly (the "break" or "truncation" radius), it's usually thought this is the result of a combination of two effects: 1) A radial threshold/cutoff in star formation, with very few stars being formed beyond a certain radius (possibly because the gas density becomes too low); and 2) Radial scattering of stars over time by spiral arms, which means that older stars tend to be scattered to larger (or smaller) radii simply because they've had more encounters with spiral arms. In this case, the relative fraction of more massive stars would *increase* with radius out to the truncation radius, and then decrease beyond.


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