Final answer:
The Roche limit is not about the maximum mass an orbiting object can have but rather the minimum distance at which a celestial body can maintain its integrity without being torn apart by tidal forces. The Chandrasekhar limit, in contrast, is related to the maximum mass a white dwarf star can have before collapsing into a neutron star or black hole.
Step-by-step explanation:
The term Roche limit actually refers to the distance within which a celestial body, due to tidal forces, will disintegrate due to the gravitational force exerted by a larger body it is orbiting. This is not directly related to the mass of the orbiting object, but rather to the distance between the two objects and the density of the orbiting object. When an object is within the Roche limit, the tidal forces can cause the object to be stretched and pulled apart, preventing it from holding itself together by its gravity alone.
Neutron stars and the concept of the Chandrasekhar limit are more related to limits on mass than the Roche limit. The Chandrasekhar limit is the upper limit to the mass of a white dwarf, which is 1.4 times the mass of the Sun. Once this limit is exceeded, the white dwarf will collapse under its own weight to form a neutron star or black hole depending on the remaining mass.
On the other hand, the text also refers to the mass constraints for main sequence stars. The lower end of the main sequence terminates where a star's mass is just enough to sustain nuclear reactions. Stars below this critical mass (about 0.075 times the mass of the Sun) are considered brown dwarfs or planets, whereas the upper limit for stellar mass is thought to be between 100 and 200 solar masses. This sets a framework for understanding the limits associated with various stages of stellar evolution.