<p>&quot;What&quot; is straightforward: L4 and L5 are two points on an orbit that are 60 degrees ahead and 60 degrees behind the planet, and so move as the planet orbits.  If the planet is less than about 1/25 of the mass of the central object, then a combination of centrifugal and Coriolis forces will cause the L4 and L5 points to be places where a third body can have a stable orbit.</p>
<p>Asteroids that have orbits at (or near) the L4 and L5 points are known as &quot;Trojans&quot; Jupiter has hundreds of Trojans that share its orbit, even Earth has one 2010 TK7 (and perhaps more).</p>
<p>&quot;Why&quot; is harder.  It seems that this is chosen to ensure that the &quot;planet&quot; is significantly smaller in mass than the central &quot;star&quot;. So that we can clearly claim that &quot;the planet orbits the star&quot; and not &quot;there are two roughly equal-sized bodies in orbit around each other&quot;.  Such configurations would be a binary system and not a planet in orbit.</p>
<p>The significance would be in the nomenclature.  In a binary (or multiple) system, the objects are named &quot;on the same level&quot; (for example Alpha-Cen A, Alpha Cen B and Alpha Cen C)  Planets, however, are named at a lower level, with lower case letters (Alpha Cen Cb) There isn't really another reason for specifying an upper limit to the size of second body.</p>
<p>It also seems to be a proxy for the mode of formation (this is hinted at by the parenthetical comment). Two roughly equal bodies will have formed by gravitational collapse of a cloud of gas that split in two as it collapsed to form two objects mutually orbiting each other.  Whereas classical &quot;planets&quot; form in the disc surrounding a proto-star as a secondary process. But rather than use the unobservable &quot;mode of formation&quot; as a definition, the IAU (in its infinte wisdom) chooses the astronomically meaningful L4/L5 instability</p>

CC BY-SA 4.0
2021-04-08T07:01:05.710Z
2021-04-08T07:01:05.710Z
James K
<p>In 2018 the <a href="https://www.iau.org/science/scientific_bodies/commissions/F2/info/documents/" rel="nofollow noreferrer">IAU produced a definition of an exoplanet</a>:</p>
<blockquote>
<p>The current official wokring definition of an <em>exoplanet</em> as amended by IAU Comission F2: Exoplanets and the Solar System in August 2018, reads as follows:</p>
<ul>
<li>Objects with true masses below the limiting mass for thermonuclear fusion of deuterium (currently calculated to be 13 Jupiter masses for objects of solare metallicity) that orbit stars, brown dwarfs or stellar remnants and that have a mass ratio with the central object below the L4/L5 instability (<span class="math-container">$M/M_{\rm central} &lt; 2/(25+ \sqrt{621})\approx 1/25 $</span>) are &quot;planets&quot; (no matter how they formed).</li>
<li>The minimal mass/ size required for an extrasolar object to be considered should be the same as that used in our Solar System.</li>
<li>We can expect this definition to evolve as our knowledge improves.</li>
</ul>
</blockquote>
<p>What is the L4/L5 instability and why was it chosen as part of the exoplanet definition?</p>

CC BY-SA 4.0
2021-04-08T06:56:06.683Z
L4 and L5 is short for [Lagrange Points 4 and 5](https://en.wikipedia.org/wiki/Lagrange_point#L4_and_L5_points).
B--rian
<exoplanet><lagrange-point><definition><iau>
IAU 2018 Exoplanet definition
sno
# IAU 2018 Exoplanet definition

(Asked by: username_0 on 2021-04-08)

In 2018 the [IAU produced a definition of an exoplanet](https://www.iau.org/science/scientific_bodies/commissions/F2/info/documents/):

> The current official wokring definition of an *exoplanet* as amended by IAU Comission F2: Exoplanets and the Solar System in August 2018, reads as follows:
>
> * Objects with true masses below the limiting mass for thermonuclear fusion of deuterium (currently calculated to be 13 Jupiter masses for objects of solare metallicity) that orbit stars, brown dwarfs or stellar remnants and that have a mass ratio with the central object below the L4/L5 instability ($M/M\_{\rm central} < 2/(25+ \sqrt{621})\approx 1/25 $) are "planets" (no matter how they formed).
> * The minimal mass/ size required for an extrasolar object to be considered should be the same as that used in our Solar System.
> * We can expect this definition to evolve as our knowledge improves.

What is the L4/L5 instability and why was it chosen as part of the exoplanet definition?

**Tags:** exoplanet, lagrange-point, definition, iau

> **Comments:**
> **username_1**: L4 and L5 is short for [Lagrange Points 4 and 5](https://en.wikipedia.org/wiki/Lagrange_point#L4_and_L5_points).  

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## 1 answers

### Answer by username_2 on 2021-04-08. Score: 3 | Accepted answer

"What" is straightforward: L4 and L5 are two points on an orbit that are 60 degrees ahead and 60 degrees behind the planet, and so move as the planet orbits. If the planet is less than about 1/25 of the mass of the central object, then a combination of centrifugal and Coriolis forces will cause the L4 and L5 points to be places where a third body can have a stable orbit.

Asteroids that have orbits at (or near) the L4 and L5 points are known as "Trojans" Jupiter has hundreds of Trojans that share its orbit, even Earth has one 2010 TK7 (and perhaps more).

"Why" is harder. It seems that this is chosen to ensure that the "planet" is significantly smaller in mass than the central "star". So that we can clearly claim that "the planet orbits the star" and not "there are two roughly equal-sized bodies in orbit around each other". Such configurations would be a binary system and not a planet in orbit.

The significance would be in the nomenclature. In a binary (or multiple) system, the objects are named "on the same level" (for example Alpha-Cen A, Alpha Cen B and Alpha Cen C) Planets, however, are named at a lower level, with lower case letters (Alpha Cen Cb) There isn't really another reason for specifying an upper limit to the size of second body.

It also seems to be a proxy for the mode of formation (this is hinted at by the parenthetical comment). Two roughly equal bodies will have formed by gravitational collapse of a cloud of gas that split in two as it collapsed to form two objects mutually orbiting each other. Whereas classical "planets" form in the disc surrounding a proto-star as a secondary process. But rather than use the unobservable "mode of formation" as a definition, the IAU (in its infinte wisdom) chooses the astronomically meaningful L4/L5 instability


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