How do I make gravitational orbits?

Hello everyone, I would like a help to know how to do realistic physics in Construct, I will give an example. I have a large circle and a small one, when the small circle approaches the big one it is pulled by gravity causing an orbit. At the same time pressing the screen applies a force to control the fall without it touching the big circle.Therefore, applying force to it is ejected out of the gravitational field and launched to another nearby circle with gravity as well. upload.wikimedia.org/wikipedia/commons/0/0d/Orbital_resonance_of_Mercury.gif

How are you looking to handle objects that approach straight on at speed? In reality these objects would never be pulled into orbit. Are you looking to force all objects to enter an orbit if they are slowed down enough?

Exactly that, imagine that when you approach the circle it will be pulled to the center but when you touch the screen it will push outwards, but if you keep pressed, it will continue to rotate around the circle

The force of gravity between objects can be done with:

F=G*m1*m2/r^2

Where

m1 and m2 are the masses of the two objects and r is the distance between them.

G is a constant. It comes from

https://en.m.wikipedia.org/wiki/Newton%27s_law_of_universal_gravitation

But since we are not dealing with real world scales we can just fudge it.

You can try the following. Also to get the moon to orbit you just have to have the perpendicular velocity high enough.

Global number a=0

Global number r=0

Global number f=0

For each planet

— set a to angle(moon.x, moon.y, planet.x, planet.y)

— set r to distance(moon.x, moon.y, planet.x, planet.y)

— set f to 100 * moon.physics.mass * planet.physics.mass/r^2

— moon: physics: apply force (f*cos(a), f*sin(a))

> The force of gravity between objects can be done with:

F=G*m1*m2/r^2

Where

m1 and m2 are the masses of the two objects and r is the distance between them.

G is a constant. It comes from

https://en.m.wikipedia.org/wiki/Newton%27s_law_of_universal_gravitation

But since we are not dealing with real world scales we can just fudge it.

You can try the following. Also to get the moon to orbit you just have to have the perpendicular velocity high enough.

Global number a=0

Global number r=0

Global number f=0

For each planet

— set a to angle(moon.x, moon.y, planet.x, planet.y)

— set r to distance(moon.x, moon.y, planet.x, planet.y)

— set f to 100 * moon.physics.mass * planet.physics.mass/r^2

— moon: physics: apply force (f*cos(a), f*sin(a))

Great explanation, I had already tried to use Newton's theory but I couldn't apply it correctly, but his explanation helped me to understand the concept and to get what I needed, thanks to everyone :D