Roche lobe

Roche lobe for an explanation of the underlying gravitational principle.

In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary.

However, for many purposes it is useful to approximate the Roche lobe as a sphere of the same volume.

The other, donor, component usually fills its Roche lobe and therefore transfers mass to the compact star.

If the star expands past its Roche lobe, then the material can escape the gravitational pull of the star.

The precise shape of the Roche lobe depends on the mass ratio, and must be evaluated numerically.

The secondary star has exceeded its Roche lobe and accreted mass to the primary star.

An object that overflows its Roche lobe will lose mass to its more massive companion.

In fact, the size of the equatorial ridge is comparable with the expected Roche lobe of the moon.

Both component stars are detached main sequence stars which do not fill their Roche lobes.

"The planet's self-gravity will hold it together as it fills its Roche lobe.

This critical equipotential defines the Roche lobes.

"Both translations - into and out of Hawking space - will be far too close to the binary system's Roche lobe.

A red supergiant fills the system's Roche lobe when closest to its companion blue star, the latter appearing to be on the main sequence.

This is a semidetached binary system where the secondary is close to filling its Roche lobe, or it may even be overflowing.

The double wave ellipsoidal light variations are produced by a tidally deformed giant that nearly fills its Roche lobe.

The Roche lobe describes the limits at which an object which is in orbit around two other objects will be captured by one or the other.

The Roche lobe is the region of space around a star in a binary system within which orbiting material is gravitationally bound to that star.

A contact binary is a type of binary star in which both components of the binary fill their Roche lobes.

If the donor star expands less rapidly or shrinks faster than its Roche lobe, mass transfer will generally be stable and may continue for a long time.

Modeling of the variations indicate strong heating of the companion by the pulsar, and that the companion nearly fills its Roche lobe.

Eventually the planet will take a teardrop shape, filling its Roche lobe, and pouring its substance down that spiral until it becomes an accretion disk.

It is so extended that the planet's radius exceeds its Roche lobe, the gravitational boundary beyond which material would be lost forever from the planet's atmosphere.

In principle, mass transfer could lead to the total disintegration of the object, since a reduction of the object's mass causes its Roche lobe to shrink.

His name was given to the concepts of the Roche sphere, Roche limit and Roche lobe.