Lagrangian point refers to a point in space at which a small body, which is experiencing the gravitational influence of two large ones, will approximately stay in a state of rest with relation to them. Furthermore, the French mathematician and astronomer Joseph-Louis Lagrange deduced the existence of such points in 1772.

**Introduction to Lagrangian Point**

Experts define the Lagrangian point as the point that is in orbit near two large bodies in such a manner that the smaller object maintains its position with relation to the large orbiting bodies. Furthermore, Lagrangian points can also be called as L point or Libration points or Lagrange points.

For every combination of two large orbital bodies, there are five Lagrangian points from L1 to L5. Furthermore, Leonhard Euler made the discovery of the first three Lagrangian points L1, L2 and L3. Also, Joseph-Louis made the discovery of Lagrangian points L4 and L5.

**Langrangian Point For Sun-Earth System**

As far as the Lagrangian point for the Sun-Earth system is concerned, there are L1 to L5 Lagrangian points. Furthermore, the formation of a line via the centre of two large bodies takes place by the Lagrangian points L1, L2, and L3. Also, the formation of an equilateral triangle with the centre of two large bodies takes place by the Langrangian points L4 and L5.

An important point to remember here is that Langrangian point stability is shown by L4 and L5. Moreover, this makes them rotate in a coordinate system whose connection is to the two large bodies. In contrast, Langrangian points L1, L2, and L3 are unstable.

**Formula of Lagrangian Point**

**L _{1} point: **The point that lies between M

_{1}and M

_{2}, which are the two large masses. Furthermore, L

_{1}lies on the line that is defined by these two large masses.

There is also partial cancellation of the gravitational attraction of M_{1} by the gravitational force of M_{2}. Below is the mathematical representation:

\(\frac{M_{1}}{\left ( R-r \right )^{2}} = \frac{M_{2}}{r^{2}} + \frac{M_{1}}{R^{2}} – \frac{r(M_{1}+M_{2})}{R^{3}}\)

Where,

- r is representative of the distance of an L
_{1}point from the smaller object - R is the distance between the two main objects
- M
_{1}and M_{2}are the masses of the large and small object

**L _{2} point: **The point that is on the line defined by the two large masses and beyond the smaller mass of the two. The balancing of the centrifugal effect on a body at L

_{2}takes place by the gravitational force of the two large masses. Furthermore, below is the mathematical representation:

\(\frac{M_{1}}{\left ( R+r \right )^{2}} + \frac{M_{2}}{r^{2}} = \frac{M_{1}}{R^{2}} + \frac{r\left ( M_{1}+M_{2} \right )}{R^{3}}\)

Where,

- r is representative of the distance of L
_{2}point from the smaller object - R is the distance that exists between the two main objects
- M
_{1}and M_{2}represent the masses of the large and small object

**L _{3} point:** The point that is on the line that is defined by the two large masses and beyond the larger mass among the two. Moreover, below is the mathematical representation:

\(\frac{M_{1}}{\left ( R-r \right )^{2}} + \frac{M_{2}}{\left ( 2R-r \right )^{2}} = \left ( \frac{M_{2}}{M_{1}+M_{2}}R+R-r \right )\frac{M_{1}+M_{2}}{R^{3}}\)

Where,

- r is representative of the distance of L
_{3}point from the smaller object - R is the distance that exists between the two main objects
- M
_{1}and M_{2}represent the masses of the large and small object

**L _{4} and L_{5} points: **These points lie on the line that experts define as between the centres of the two masses in such a manner that they are at the third corner of the two equilateral triangles. Moreover, below is the mathematical representation by making use of radial acceleration:

a = \(\frac{-GM_{1}}{r^{2}}sgn\left ( r \right ) + \frac{GM_{2}}{\left ( R-r \right )^{2}}sgn\left ( R-r \right ) + \frac{G\left ( \left ( M_{1}+M_{2} \right )r-M_{2}R \right )}{R^{3}}\)

Where,

- a represents the radial acceleration
- r refers to the distance from the large body M1
- sgn (x) is x’s sign function

**FAQs For Langrangian Point**

**Question 1: How many lagrangian points are there in space according to Physics?**

**Answer 1:** As far as space is concerned, one can take a look at the Sun-Earth System. Here, the Lagrangian points are L1 to L5. Most noteworthy, the Langrangian points L1, L2, and L3 are unstable while the Langrangian points L4 and L5 are stable.

**Question 2: Give a mathematical expression for Langrangian points L4 and L5?**

**Answer 2:** The mathematical expression for Langrangian points L4 and L5 is a = \(\frac{-GM_{1}}{r^{2}}sgn\left ( r \right ) + \frac{GM_{2}}{\left ( R-r \right )^{2}}sgn\left ( R-r \right ) + \frac{G\left ( \left ( M_{1}+M_{2} \right )r-M_{2}R \right )}{R^{3}}\).

Here, a refers to the radial acceleration and r refers to the distance from the large body M1. Also, sgn (x) is x’s sign function.

When earth is near know it move faster some gravity of earth act on it and it produce restriction so speed may be slownear sun

When earth is near the sun how it move faster some gravity of sun act on it and it produce restriction and speed may be slow down