<p>Nice question and interesting data! Going through the references of the linked site, one gets a more verbose description of the <a href="https://www.eso.org/public/videos/eso0411a/" rel="noreferrer">video</a>:</p>
<blockquote>
<p>After more than 1,000 nights of observations spread over 15 years, they have determined the spatial motions of more than 14,000 solar-like stars residing in the neighbourhood of the Sun.</p>
</blockquote>
<blockquote>
<p>For the first time, the changing dynamics of the Milky Way since its birth can now be studied in detail and with a stellar sample sufficiently large to allow a sound analysis. The astronomers find that our home galaxy has led a much more turbulent and chaotic life than previously assumed.</p>
</blockquote>
<blockquote>
<p>ESO Press Video eso0411 shows the stars studied during the present programme making their most recent orbital revolution around the Galactic centre before converging into the small volume where they were observed by the team. The duration of the video corresponds to about 250 million years. The yellow dot and white curve show how the Sun moved during this last of its about 20 laps around our Galaxy.</p>
</blockquote>
<p>So this video shows the last orbit of the observed stars in the solar vicinity, starting at about one Galactic year ago, ending in the present state. In the press release they also link the <a href="https://www.aanda.org/articles/aa/pdf/2004/18/aa0959.pdf" rel="noreferrer">paper</a> by Nordström et al. with the scientific analysis which allowed them to create this backward propagation of peculiar motion of these stars.</p>
<p>In figure 30 they show the velocity distribution of the observed stars in the components U,V,W - a pretty uniform distribution, even when they can make out some distinct populations. So these stars with the &quot;strange&quot; orbits can be any or all of this: stars with very elliptic or high galactic latitude orbits (which thus only project to very elliptic in this face-on view of the disk. As to the reasons of these comparatively disturbed orbits they write in the summary, speaking about kinematic heating of the stellar orbits due to external influences:</p>
<blockquote>
<p>Mühlbauer &amp; Dehnen (2003) however, show
that when the true velocity dispersion and non-axisymmetric
disturbances of the disk are taken into account, large variations [in the velocities] can occur. The smaller exponents for the in-disk heating (<span class="math-container">$σ_U$</span> , <span class="math-container">$σ_V$</span> ) compared to the out-of-the-disk heating (<span class="math-container">$σ_W$</span> )
gives further constraints to be fulfilled by models trying to ex-
plain the observed kinematic heating of the disk. At least four
mechanisms have been proposed to explain the heating: fast perturbers from the halo, such as <span class="math-container">$10^6 M_\circ$</span> black holes; slow perturbers in the disk, such as giant molecular clouds; large scale perturbations of the disk caused by spiral arms (De Simone et al. 2004) or the bar (e.g. Fux 2001); and finally heating
caused by infalling satellite galaxies.</p>
</blockquote>
<p>Mind also that these few stars which stick out with their orbits in this kind of plot or animation are very few compared to the overall number of investigated stars of 11k to 12k. They are over- emphasised as the dots of the normal - behaving stars overlap without transparency.</p>

CC BY-SA 4.0
2022-06-07T21:14:26.510Z
2022-06-08T06:47:06.947Z
2022-06-08T06:47:06.947Z
planetmaker
<p>I found this GIF by the European Southern Observatory (ESO) in the Wikipedia article on the <a href="https://en.wikipedia.org/wiki/Galactic_year" rel="nofollow noreferrer">galactic year</a>, with the following description:</p>
<blockquote>
<p>Visualisation of the orbit of the Sun (yellow dot and white curve) around the Galactic Centre (GC) in the last galactic year. The red dots correspond to the positions of the stars studied by the European Southern Observatory in a monitoring programme.</p>
</blockquote>
<p><a href="https://i.sstatic.net/QnaoI.gif" rel="nofollow noreferrer"><img src="https://i.sstatic.net/QnaoI.gif" alt="enter image description here" /></a></p>
<p>To the extent I understand, the red dots are stars in our galaxy. We can see their movement over one galactic year. Careful observation will reveal that there are stars that appear to simply move from left to right through the galactic center until they are out of the frame. <strong>What are they?</strong> I thought of 3 options (none of which I like):</p>
<ol>
<li>stars with high eccentricity</li>
<li>intergalactic stars</li>
<li>simply stars that seem to pass through the GC but really have about 90° inclination to the Sun's path plane, hence in this 2d projection they appear as such.</li>
</ol>

CC BY-SA 4.0
2022-06-08T11:21:13.747Z
and 4. Stars that had a recent close encounter with something heavy and just appear to come from the GC, but never actually were there but extrapolation of their orbits failed.
asdfex
<star><galaxy><milky-way>
What are those stars that cross the galactic center?
d_e
# What are those stars that cross the galactic center?

(Asked by: username_0 on 2022-06-07)

I found this GIF by the European Southern Observatory (ESO) in the Wikipedia article on the [galactic year](https://en.wikipedia.org/wiki/Galactic_year), with the following description:

> Visualisation of the orbit of the Sun (yellow dot and white curve) around the Galactic Centre (GC) in the last galactic year. The red dots correspond to the positions of the stars studied by the European Southern Observatory in a monitoring programme.

[![enter image description here](https://i.sstatic.net/QnaoI.gif)](https://i.sstatic.net/QnaoI.gif)

To the extent I understand, the red dots are stars in our galaxy. We can see their movement over one galactic year. Careful observation will reveal that there are stars that appear to simply move from left to right through the galactic center until they are out of the frame. **What are they?** I thought of 3 options (none of which I like):

1. stars with high eccentricity
2. intergalactic stars
3. simply stars that seem to pass through the GC but really have about 90° inclination to the Sun's path plane, hence in this 2d projection they appear as such.

**Tags:** star, galaxy, milky-way

> **Comments:**
> **username_1**: and 4. Stars that had a recent close encounter with something heavy and just appear to come from the GC, but never actually were there but extrapolation of their orbits failed.  

---

## 1 answers

### Answer by username_2 on 2022-06-07. Score: 10 | Accepted answer

Nice question and interesting data! Going through the references of the linked site, one gets a more verbose description of the [video](https://www.eso.org/public/videos/eso0411a/):

> After more than 1,000 nights of observations spread over 15 years, they have determined the spatial motions of more than 14,000 solar-like stars residing in the neighbourhood of the Sun.

> For the first time, the changing dynamics of the Milky Way since its birth can now be studied in detail and with a stellar sample sufficiently large to allow a sound analysis. The astronomers find that our home galaxy has led a much more turbulent and chaotic life than previously assumed.

> ESO Press Video eso0411 shows the stars studied during the present programme making their most recent orbital revolution around the Galactic centre before converging into the small volume where they were observed by the team. The duration of the video corresponds to about 250 million years. The yellow dot and white curve show how the Sun moved during this last of its about 20 laps around our Galaxy.

So this video shows the last orbit of the observed stars in the solar vicinity, starting at about one Galactic year ago, ending in the present state. In the press release they also link the [paper](https://www.aanda.org/articles/aa/pdf/2004/18/aa0959.pdf) by Nordström et al. with the scientific analysis which allowed them to create this backward propagation of peculiar motion of these stars.

In figure 30 they show the velocity distribution of the observed stars in the components U,V,W - a pretty uniform distribution, even when they can make out some distinct populations. So these stars with the "strange" orbits can be any or all of this: stars with very elliptic or high galactic latitude orbits (which thus only project to very elliptic in this face-on view of the disk. As to the reasons of these comparatively disturbed orbits they write in the summary, speaking about kinematic heating of the stellar orbits due to external influences:

> Mühlbauer & Dehnen (2003) however, show
> that when the true velocity dispersion and non-axisymmetric
> disturbances of the disk are taken into account, large variations [in the velocities] can occur. The smaller exponents for the in-disk heating ($σ\_U$ , $σ\_V$ ) compared to the out-of-the-disk heating ($σ\_W$ )
> gives further constraints to be fulfilled by models trying to ex-
> plain the observed kinematic heating of the disk. At least four
> mechanisms have been proposed to explain the heating: fast perturbers from the halo, such as $10^6 M\_\circ$ black holes; slow perturbers in the disk, such as giant molecular clouds; large scale perturbations of the disk caused by spiral arms (De Simone et al. 2004) or the bar (e.g. Fux 2001); and finally heating
> caused by infalling satellite galaxies.

Mind also that these few stars which stick out with their orbits in this kind of plot or animation are very few compared to the overall number of investigated stars of 11k to 12k. They are over- emphasised as the dots of the normal - behaving stars overlap without transparency.


---

