The objects with a speed higher v = 7668 m/s than that number are likely to go into orbit. (Y & Z)
The orbital speed of an astronomical body or object (e.g. planet, moon, artificial satellite, spacecraft, or star) is the speed at which it orbits around either the barycenter or if one object is much more massive than the other bodies in the system, its speed relative to the centre of mass of the most massive body.
The term can be used to refer to either the mean orbital speed, i.e. the average speed over an entire orbit, or its instantaneous speed at a particular point in its orbit.
Maximum (instantaneous) orbital speed occurs at periapsis (perigee, perihelion, etc.), while minimum speed for objects in closed orbits occurs at apoapsis (apogee, aphelion, etc.).
In ideal two-body systems, objects in open orbits continue to slow down forever as their distance to the barycenter increases.
g = v^2 / r
so v = square root ( r x g )
v = 7668 m/s will be the minimum speed needed to go into orbit.
Based on that, objects with a speed higher than that number are likely to go into orbit. (Y & Z)
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