The Milky Way galaxy, a swirling island of stars, gas, and dust, isn't as static as it appears. Beneath the surface of predictable orbits lies a hidden dynamic: stars can be ejected from the galactic center, flung outwards at incredible speeds. Recent research is focusing not on the *fastest* of these ejected stars, but on a slower, more subtle population that could significantly impact our understanding of the galaxy's structure and evolution.This article delves into the science behind stellar ejection, the mechanisms driving it, and the implications of discovering these slower-moving galactic exiles.

The dynamics of celestial bodies are frequently enough simplified for calculation. Two-body systems (like the Earth and Sun) have well-defined solutions.Though,the moment a third body enters the equation,the system becomes incredibly complex. This is known as the 3-body problem. There's no general closed-form solution; predicting the long-term behavior requires complex simulations. These simulations reveal a surprising outcome: in multi-body systems, objects can be ejected. Gravity, while always attractive, can lead to chaotic interactions where one object gains enough energy to escape the gravitational pull of the others.

At the heart of our galaxy lies Sagittarius A* (Sgr A*), a supermassive black hole with a mass over four million times that of our Sun. Astronomers have long suspected that sgr A* plays a role in ejecting stars. The hills mechanism describes a process where a binary star system passing near Sgr A* can be disrupted. One star gets captured by the black hole,while the other is flung outwards at tremendous speed.This process can launch stars at speeds up to 3,500 kilometers per second - approximately 13 million km/hr (8 million mph)!

While high-velocity stars ejected via the Hills mechanism have been observed, a team of astronomers recently focused on a more elusive population: stars ejected at slower