<p>I assume you are referring to the rotation curve of galaxies, i.e. the speed of matter (stars, gas clouds, etc.) as a function of its distance from the center. This speed will depend on the <em>matter distribution</em>, that is, how the galaxies' constituents are distributed throughout the galaxies.</p>

<p><strong>Keplerian rotation</strong></p>

<p>If (almost) all of the mass $M$ were located in the center, then a star at a distance $R$ would have a speed $V = \sqrt{GM/R}$. This is called <em>Keplerian rotation</em>, because this is how planets in the Solar system move, which were described by Johannes Kepler. In this case, the mass inside a radius $R$ is (almost) constant, i.e. $M'(&lt;R) = M$.</p>

<p><strong>Flat rotation</strong></p>

<p>Most disk galaxies have a large concentration of visible mass in the center (the "bulge"), so one might think that Keplerian rotation would be a good description of the stars' speeds. But this is not what is observed. In fact, the speed is seen to rise steeply the first few kpc, and then stay constant out to distances where no light is detected. This will happen if the mass $M'(&lt;R)$ inside $R$ increases with $R$, i.e. if the matter is distributed throughout the galaxy. This is one of several pieces of evidence that 1) there exists some matter that we cannot see, in addition to what we <em>can</em> see, 2) that this matter dominates the kinematics of the galaxies, and 3) that it resides in a halo that extends beyond the visible matter. We call it dark matter.</p>

<p><strong>Solid body rotation</strong></p>

<p>If in addition to a given matter distribution the distances between the individual parts are fixed, the object we are discussing would describe a solid body. Of course this can't be the case for a galaxy, but it will be the case for a rocky planet. In this case the velocity of a given point will depend linearly on its perpendicular distance to the axis of rotation, i.e. $V \propto R$.</p>

<p><strong>Density profile of the matter distribution</strong></p>

<p>Excactly <em>how</em> the matter is distributed in the galaxy is not easily deducted, and varies from galaxy type to galaxy type. An early description of the matter density as a function of distance from the center was the so-called <a href="https://en.wikipedia.org/wiki/Navarro%E2%80%93Frenk%E2%80%93White_profile" rel="nofollow noreferrer">NFW profile</a>, but other models may be better, e.g. a <a href="https://en.wikipedia.org/wiki/Sersic_profile" rel="nofollow noreferrer">Sérsic profile</a> or an <a href="https://en.wikipedia.org/wiki/Einasto_profile" rel="nofollow noreferrer">Einasto profile</a>.</p>

<p>So, to summarize, <strong>the term "matter distribution" refers to density as a function of location, i.e. $\rho(\mathbf{r})$, for some object</strong>. This can be for any object — solid, liquid, gaseous, or consisting of several components that are held together by gravity — but in any case it is true that its form determines its rotation, and the three different rotation forms you mention are often discussed in the context of galaxies.</p>

<hr>

<p>The three different cases are illustratred below. Keplerian, solid, and flat rotation are drawn in green, red, and blue, respectively. For comparison, a typical spiral galaxy velocity curve is drawn in magenta.</p>

<p><a href="https://i.sstatic.net/m7UyF.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/m7UyF.png" alt="rotation"></a></p>

CC BY-SA 3.0
2015-10-24T15:15:30.140Z
I wasn't referring to anything, if you read my question it is a term I am unfamilar with...! That is why I was asking.
MichaelJRoberts
CC BY-SA 3.0
2015-10-24T16:41:00.043Z
Yes yes, I meant nothing by it, I just wasn't excactly sure, so I wanted to describe how I interpreted your question.
pela
CC BY-SA 3.0
2015-10-24T19:16:35.277Z
@MichaelJRoberts: I edited my answer a bit. Does it make sense now?
pela
CC BY-SA 3.0
2015-10-24T20:03:35.857Z
I'm quite happy with the flat roation matter distribution, am I right in saying that matter is increasing w.r.t to radius? Also, w.r.t to solid body rotation, are we assuming the mass is equally distributed in say a disc? Or could it be evenly distributed throughout a sphere...(both cases the distance between stars/particles is fixed?)
MichaelJRoberts
CC BY-SA 3.0
2015-10-24T23:17:00.770Z
Maybe semantics, but I wouldn't say that _matter_ is increasing (for flat rotation), but the _mass_ in side a sphere of radius $R$ increases with $R$, because you keep enclosing more mass, the larger you make your sphere. In contrast, for Keplerian rotation, all the matter/mass is in the center, so no matter how large you make your sphere, the total mass doesn't increase.
pela
CC BY-SA 3.0
2015-10-24T23:24:16.467Z
Wrt. solid body rotation, the matter can be distributed in many ways. The term just means that the body's consituents don't move with respect to each other. For instance, a rocky planet is spherical, and usually more dense in the center, while a billiard ball is spherical with a uniform density distribution. A coin is disky with a uniform density distribution. All three are examples of solid bodies (ignoring that some rocky planets, e.g. Earth, have a liquid core). A galaxy cannot be a solid body, since the stars etc. _do_ move with respect to each other.
pela
CC BY-SA 3.0
2015-10-27T12:08:26.517Z
@MichaelJRoberts if this doesn't answer your question, maybe I misunderstand you. Let me know what's unclear, and I can try and fix it.
pela
CC BY-SA 3.0
2015-10-21T22:11:00.287Z
2015-10-25T09:22:16.393Z
2015-10-25T09:22:16.393Z
pela
<p>A distribution is a function mapping from one (or more) variables onto other  (often a single, usually non-negative) variable(s). Generally, matter distribution is the relationship between location and mass density (sometimes averages over macroscopic distances, sometimes objects which are assumed to be point masses). Typically in astronomy the radial distance from some center point is the (most significant) independent variable. You should have some familiarity with euclidean, polar, conical, and spherical coordinate systems. Most 'well behaved' distributions → 0 as distance → ∞.</p>

CC BY-SA 3.0
2016-07-03T19:16:23.483Z
2016-07-03T19:16:23.483Z
Li Zhi
<p>Frustratingly, I find this could be a very simplistic question and may leave me feeling a little stupid for asking it. But I have to ask this.</p>

<p>My lecturer keeps refering to "matter distributions" for various rotation cases, e.g., Keplerian rotation, solid body rotation, flat rotation etc etc. </p>

<p>I was wondering if anyone knew exactly what this term means, or the specifics for each case?</p>

<orbit><galaxy><rotation>
What is meant by matter distribution?
MichaelJRoberts
# What is meant by matter distribution?

(Asked by: username_0 on 2015-10-21)

Frustratingly, I find this could be a very simplistic question and may leave me feeling a little stupid for asking it. But I have to ask this.

My lecturer keeps refering to "matter distributions" for various rotation cases, e.g., Keplerian rotation, solid body rotation, flat rotation etc etc.

I was wondering if anyone knew exactly what this term means, or the specifics for each case?

**Tags:** orbit, galaxy, rotation

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## 2 answers

### Answer by username_1 on 2015-10-21. Score: 5

I assume you are referring to the rotation curve of galaxies, i.e. the speed of matter (stars, gas clouds, etc.) as a function of its distance from the center. This speed will depend on the *matter distribution*, that is, how the galaxies' constituents are distributed throughout the galaxies.

**Keplerian rotation**

If (almost) all of the mass $M$ were located in the center, then a star at a distance $R$ would have a speed $V = \sqrt{GM/R}$. This is called *Keplerian rotation*, because this is how planets in the Solar system move, which were described by Johannes Kepler. In this case, the mass inside a radius $R$ is (almost) constant, i.e. $M'(

**Flat rotation**

Most disk galaxies have a large concentration of visible mass in the center (the "bulge"), so one might think that Keplerian rotation would be a good description of the stars' speeds. But this is not what is observed. In fact, the speed is seen to rise steeply the first few kpc, and then stay constant out to distances where no light is detected. This will happen if the mass $M'(can see, 2) that this matter dominates the kinematics of the galaxies, and 3) that it resides in a halo that extends beyond the visible matter. We call it dark matter.

**Solid body rotation**

If in addition to a given matter distribution the distances between the individual parts are fixed, the object we are discussing would describe a solid body. Of course this can't be the case for a galaxy, but it will be the case for a rocky planet. In this case the velocity of a given point will depend linearly on its perpendicular distance to the axis of rotation, i.e. $V \propto R$.

**Density profile of the matter distribution**

Excactly *how* the matter is distributed in the galaxy is not easily deducted, and varies from galaxy type to galaxy type. An early description of the matter density as a function of distance from the center was the so-called [NFW profile](https://en.wikipedia.org/wiki/Navarro%E2%80%93Frenk%E2%80%93White_profile), but other models may be better, e.g. a [Sérsic profile](https://en.wikipedia.org/wiki/Sersic_profile) or an [Einasto profile](https://en.wikipedia.org/wiki/Einasto_profile).

So, to summarize, **the term "matter distribution" refers to density as a function of location, i.e. $\rho(\mathbf{r})$, for some object**. This can be for any object — solid, liquid, gaseous, or consisting of several components that are held together by gravity — but in any case it is true that its form determines its rotation, and the three different rotation forms you mention are often discussed in the context of galaxies.

---

The three different cases are illustratred below. Keplerian, solid, and flat rotation are drawn in green, red, and blue, respectively. For comparison, a typical spiral galaxy velocity curve is drawn in magenta.

[![rotation](https://i.sstatic.net/m7UyF.png)](https://i.sstatic.net/m7UyF.png)

> **Comments:**
> **username_0**: I wasn't referring to anything, if you read my question it is a term I am unfamilar with...! That is why I was asking.  
> **username_1**: Yes yes, I meant nothing by it, I just wasn't excactly sure, so I wanted to describe how I interpreted your question.  
> **username_1**: @MichaelJRoberts: I edited my answer a bit. Does it make sense now?  
> **username_0**: I'm quite happy with the flat roation matter distribution, am I right in saying that matter is increasing w.r.t to radius? Also, w.r.t to solid body rotation, are we assuming the mass is equally distributed in say a disc? Or could it be evenly distributed throughout a sphere...(both cases the distance between stars/particles is fixed?)  
> **username_1**: Maybe semantics, but I wouldn't say that _matter_ is increasing (for flat rotation), but the _mass_ in side a sphere of radius $R$ increases with $R$, because you keep enclosing more mass, the larger you make your sphere. In contrast, for Keplerian rotation, all the matter/mass is in the center, so no matter how large you make your sphere, the total mass doesn't increase.  
> **username_1**: Wrt. solid body rotation, the matter can be distributed in many ways. The term just means that the body's consituents don't move with respect to each other. For instance, a rocky planet is spherical, and usually more dense in the center, while a billiard ball is spherical with a uniform density distribution. A coin is disky with a uniform density distribution. All three are examples of solid bodies (ignoring that some rocky planets, e.g. Earth, have a liquid core). A galaxy cannot be a solid body, since the stars etc. _do_ move with respect to each other.  
> **username_1**: @MichaelJRoberts if this doesn't answer your question, maybe I misunderstand you. Let me know what's unclear, and I can try and fix it.  

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### Answer by username_2 on 2016-07-03. Score: 1

A distribution is a function mapping from one (or more) variables onto other (often a single, usually non-negative) variable(s). Generally, matter distribution is the relationship between location and mass density (sometimes averages over macroscopic distances, sometimes objects which are assumed to be point masses). Typically in astronomy the radial distance from some center point is the (most significant) independent variable. You should have some familiarity with euclidean, polar, conical, and spherical coordinate systems. Most 'well behaved' distributions → 0 as distance → ∞.


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