If the orbiting body's mass is a significant fraction of the central body's mass, the weak stability boundaries can be more dramatic. 

Call the mass of the central body + orbiting body 1. Call the orbiting body's mass µ. Then the central body would have mass 1-µ.

Here are pairs arranged in order of µ


Pluto/Charon 1.043E-01  
Earth/Moon 1.216E-02  
Sun/Jupiter 9.545E-04  
Sun/Saturn 2.856E-04  
Saturn/Titan 2.374E-04  
Jupiter/Ganymede 7.789E-05  
Jupiter/Callisto 5.684E-05  
Sun/Neptune 5.153E-05  
Jupiter/Io 4.700E-05  
Sun/Uranus 4.366E-05  
Jupiter/Europa 2.526E-05  
Saturn/Rhea 4.046E-06  
Sun/Earth 3.039E-06  
Sun/Venus 2.448E-06  
Saturn/Dione 1.935E-06  
Saturn/Tethys 1.091E-06  
Sun/Mars 3.229E-07  
Saturn/Enceladus 1.935E-07  
Sun/Mercury 1.659E-07  
Saturn/Mimas 7.037E-08  
Mars/Phobos 1.682E-08  
Sun/Pluto& Charon 7.149E-09  
Mars/Deimos 2.803E-09  
Sun/Ceres 4.741E-10

Jupiter and Saturn have some big moons. You'll find a lot of the gas giant moons near the top of the list when arranged by µ.

For more on this see my [mass parameter and ITN](https://hopsblog-hop.blogspot.com/2015/06/mass-parameter-and-itn.html)