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Topic: Roche lobe

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Roche limit

Hill sphere

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Lagrangian point

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	Roche lobe
		The volume around a star in a binary system in which, if you were to release a particle, it would fall back onto the surface of that star.
		The point at which the Roche lobes of the two stars touch is called the inner Lagrangian point.
		If a star in a close binary system evolves to the point at which it fills its Roche lobe, calculations predict that material from this star will overflow both onto the companion star (via the L1 point) and into the environment around the binary system.
	www.daviddarling.info /encyclopedia/R/Roche_lobe.html (171 words)

	Roche lobe - Wikipedia, the free encyclopedia
		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.
		This is not derivable from the Roche lobe model as the coriolis force is a non-conservative force (i.e.
		Overflow from the Roche lobe is responsible for a number of astronomical phenomena, including recurring novae (binary stars consisting of a red giant and a white dwarf that are sufficiently close enough together that material from the red giant dribbles down onto the white dwarf), X-ray binaries and millisecond pulsars.
	en.wikipedia.org /wiki/Roche_lobe (592 words)

	Roche limit - Wikipedia, the free encyclopedia (Site not responding. Last check: 2007-10-26)
		The Roche limit, sometimes referred to as the Roche radius, is the distance within which a celestial body held together only by its own gravity will disintegrate due to a second celestial body's tidal forces exceeding the first body's gravitational self-attraction.
		The Roche limit should not be confused with the concept of the Roche lobe, which is also named after Édouard Roche.
		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.
	www.sciencedaily.com /encyclopedia/roche_limit (1335 words)

	NationMaster - Encyclopedia: Roche limit (Site not responding. Last check: 2007-10-26)
		The Roche limit is the distance within which a celestial body held together only by its own gravity will disintegrate due to a second celestial body's tidal forces exceeding the first body's gravitational self-attraction.
		Earth’s Roche limit for comets is 34,700 km or 5.43 radii and for asteroids, 19,000 km or 2.98 radii.
		The table in the Roche limits for selected examples section showing where various solar system bodies are relative to their roche limits mixes ratios and percentages.
	www.nationmaster.com /encyclopedia/Roche-limit (3026 words)

	Learn more about Roche limit in the online encyclopedia. (Site not responding. Last check: 2007-10-26)
		The Roche limit is sometimes described in terms of "Roche lobes", a three-dimensional mathematical surface which forms a two-lobed figure-eight shape with each of the two masses at the center of its respective lobe.
		If you were to hypothetically fill these lobes completely with water a ship could sail from one mass to the other, passing through a point between the two where both planet-wide oceans touch the tips of their sharp peaks together.
		Recurring novas are a white dwarf/red giant binary star where they are close enough together that the red giant overflows its Roche lobe and dribbles outer material down onto the white dwarf.
	www.onlineencyclopedia.org /r/ro/roche_limit.html (503 words)

	Lobe - Wikipedia, the free encyclopedia
		A pair of channels between a data station and a lobe attaching unit, one channel for sending and one for receiving, as seen from the point of view of the attached data station.
		More generally, a lobe may refer to divisions of an organ or other unit, such as the lobes of the lung and the liver.
		In astronomy, 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
	en.wikipedia.org /wiki/Lobe (230 words)

	Roche limit (Site not responding. Last check: 2007-10-26)
		The Roche limit is the distance within which an idealised moon, held together only by gravity, will start to disintegrate due to tidal force s exceeding its gravitational self-attraction.
		Real satellite s, both natural and artificial, can usually orbit within their Roche limits because they are held together by forces other than gravitation (primarily the tensile strength s of their materials).
		The Roche limit is sometimes described in terms of " Roche lobe s", a three-dimensional mathematical surface which forms a two-lobed figure-eight shape with each of the two masses at the center of its respective lobe.
	www.serebella.com /encyclopedia/article-Roche_limit.html (601 words)

	Roche lobe: Facts and details from Encyclopedia Topic (Site not responding. Last check: 2007-10-26)
		The roche limit is the distance within which a celestial body held together only by its own gravity will disintegrate due to a second celestial bodys tidal forces...
		This is not derivable from the Roche lobe model as the coriolis force is a non-conservative force conservative force quick summary:
		A nova is a cataclysmic nuclear explosion caused by the accretion of hydrogen onto the surface of a white dwarf star....
	www.absoluteastronomy.com /encyclopedia/r/ro/roche_lobe.htm (1569 words)

	Roche lobe drawing routine
		Roche is a visualization and analysis tool for drawing the Roche-lobe grometry of evolving binaries.
		Roche can be used as a standalone program reading data from the command line or from a file generated by
		Roche creates a series of images, based on the SeBa output file SeBa.data, displayin the evolutionary state of a binary.
	www.manybody.org /manybody/roche.html (299 words)

	Roche lobe (Site not responding. Last check: 2007-10-26)
		The Roche lobe is the region of space around star in a binary system within which orbiting material is gravitationally to that star.
		If the star expands its Roche lobe then the material outside the lobe will fall into the other It is approximately tear-drop shaped with the of the tear-drop pointing towards the other (and the apex is at the Lagrange L1 point of the system).
		This is not derivable from the lobe model as the coriolis force is non- conservative force (i.e.
	www.freeglossary.com /Roche_lobe (308 words)

	Temporal Lobe Seizure -- Recommendations and Resources (Site not responding. Last check: 2007-10-26)
		The parietal lobe is a lobe in the brain.
		The frontal lobe comprises four major folds of cortical tissue: the precentral gyrus, superior gyrus and the middle gyrus of the frontal gyri, the inferior frontal gyrus.
		People who have damaged frontal lobes may experience problems with these aspects of cognitive function, being at times impulsive; impaired in their ability to plan and execute complex sequences of actions; perhaps persisting with one course of action or pattern of behaviour when a change would be appropriate (perseveration).
	www.becomingapediatrician.com /health/145/temporal-lobe-seizure.html (1381 words)

	Interpretation of a Doppler Map
		With the assumption of synchronous stellar rotation around the center of mass, the Roche lobes of the stellar components are undistorted when translated to the velocity map.
		The solid-line trajectory, extending left of the secondary star's Roche lobe, is the free-fall velocity path of the stream, while the dashed-line trajectory is the Keplerian image of this path.
		5.3, the solid-line trajectory that extends to the left of the secondary star's Roche lobe is the predicted ballistic (or free-fall) trajectory of the stream in velocity space.
	mintaka.sdsu.edu /faculty/quyen/node24.html (1085 words)

	Chapter 20, Section 6 (Site not responding. Last check: 2007-10-26)
		The two teardrop-shaped regions are called Roche lobes, after Edouard Roche, the French mathematician who first studied the binary-system problem in the nineteenth century and whose work we have already encountered in the context of planetary rings.
		The greater the mass of one component, the larger is its Roche lobe and the farther from its center (and the closer to the other star) is the Lagrange point.
		Normally, both stars lie well within their respective Roche lobes, and such a binary system is said to be detached, as in Figure 20.22(a).
	astronomy.nju.edu.cn /astron/AT3/AT32006.HTM (1566 words)

	Binary star - Wikipedia, the free encyclopedia
		As a main sequence star increases in size during its evolution, it may at some point exceed its Roche lobe, meaning that some of its matter ventures into a region where the gravitational pull of its companion star is larger than its own.
		If a star grows outside of its Roche lobe too fast for all abundant matter to be transferred to the other component, it is also possible that matter will leave the system through other Lagrange points, thus being effectively lost to both components.
		The paradox can be solved by mass transfer: when the more massive star became a subgiant, it filled its Roche lobe, and most of the mass was transferred to the other star, which is still in the main sequence.
	www.wikipedia.org /wiki/Semidetached_binary (4436 words)

	The Solar System Encyclopaedia — R
		Earth's Roche lobe is at 18,470 km (2.9 Earth radii).
		It is interesting to note that the rings of the gas giants are within the Roche limit of the planet and those zones are devoid of any moons (except maybe for the tiny ones closest to the planet...).
		It remains unknown whether planetary rings are remnants of any larger satellite or satellites or whether they were formed simultanously with the planet and their particles could not clump into larger moons due to the gravity close to the planet (just like giant Jupiter prevented asteroids from collecting together to form a planet)
	ksiezyce.republika.pl /encyclopaedia/r_en.html (339 words)

	4.1 Binary evolution
		The gravitational potential of the binary system is described by the Roche model where each star dominates the gravitational potential inside regions called Roche lobes.
		The two Roche lobes meet at the inner Lagrange point along the line joining the two stars.
		Roche lobe overflow can be triggered by the evolution of the binary properties or by evolution of the component stars.
	relativity.livingreviews.org /Articles/lrr-2006-2/articlesu8.html (1089 words)

	X-ray Binaries
		The Roche lobe of an object is the volume around the object, inside which material is gravitationally bound to that object.
		The point between Roche lobes in a binary system is where the gravity from the companion is equal to the gravity from the compact object.
		It often happens that this point is close to the companion's surface, so that some of the material in the star's outer edges (on the edge of the Roche lobe) finds itself no longer bound to the star.
	www.airynothing.com /high_energy_tutorial/sources/binaries.html (662 words)

	Roche limit
		The Roche limit is sometimes described in terms of " Roche lobes ", athree-dimensional mathematical surface which forms a two-lobed figure-eight shape with each of the two masses at the center ofits respective lobe.
		If you were to hypotheticallyfill these lobes completely with water a ship could sail from one mass to the other, passing through a point between the twowhere both planet-wide oceans touch the tips of their sharp peaks together.
		Planetary rings are always located within their Roche limit, whichprevents their component particles from coalescing into one or more larger bodies.
	www.therfcc.org /roche-limit-34735.html (400 words)

	Slide 1
		The Roche surface is, therefore, the surface along which the gravitational potential is common between the stars.
		Once a star fills its Roche lobe, gas moves into the Roche lobe of the companion star and is pulled in toward that star.
		During Roche lobe overflow, mass transfer feeds gas particles in the stream from the inner Lagrangian point (L1), where the two Roche lobes touch.
	www.udayton.edu /~physics/jee/PHY250/LectureSlides/Part4/Nova_files/slide0005.htm (219 words)

	Planetary systems and their changing theories
		The empty circle on the right is approximately the size of the Roche lobe of the planet.
		Thus, we begin to resolve the structure in gas flowing into the white oval, representing the sphere of influence or Roche lobe of the planet.
		The wakes are seen on both sides of the Roche lobe, resembling in nature the keel-water of a boat or a shock wave behind a supersonic plane (of course most of the disk does rotate supersonically with respect to the planet).
	www.astro.su.se /~pawel/blois/talk_3.3.1.html (1383 words)

	Roche Model
		In the mid-nineteenth century, the mathematician Edouard Albert Roche unknowingly laid down the foundations required to describe the stellar configurations in binary systems.
		With this assumption, the ``Roche model'' describes the gravitational equilibrium surfaces around two point masses, which are distorted because of rotation and tidal forces.
		If both components fill their Roche lobe or extend beyond their Roche lobes, the binary is a contact system, in which case, a common envelope surrounds both stars.
	mintaka.sdsu.edu /faculty/quyen/node10.html (835 words)

	Roche Lobe
		The Roche lobe is a volume around a star in a binary system, inside which material is bound to that star.
		At the surface of the Roche lobe, counteracting gravitational forces due to both stars effectively cancel each other out.
		The red line in the following figure represents the equipotential surface of the Roche lobe in a HMXB (left) and LMXB (right).
	www.astro.northwestern.edu /~lin/glossary/Rochelobe.html (96 words)

	distinguishing MOND from dark matter
		The Roche lobe volume is proven to scale linearly with the baryonic mass ratio which applies to any modification function mu(g) or power-law function zeta.
		The lobes are squashed, with the aspect ratio varying with mu(g) due to the anisotropic dilation effect in MOND-like gravity.
		We prove analytically that the Roche lobe volume scales linearly with the "true" baryonic mass ratio in both Newtonian and deep-MOND regimes, insensitive to the modification to the inertia mass.
	www.physicsforums.com /showthread.php?t=101707 (2469 words)

	Astron. Astrophys. 321, 207-212 (1997)
		Lower limit to the initial semi-major axis at which the binary survives the spiral-in, as function of the initial mass of the primary, calculated with use of the evolutionary sequences by Schaller et al.
		Romani 1992 mentions the possibility that the secondary star might fill its Roche lobe as it evolves on the asymptotic giant-branch after the primary collapsed into a remnant without ever having reached Roche-lobe contact.
		It is seen that this semi-major axis is so small, that it invalidates the assumption that Roche lobe contact of the primary has been avoided.
	aa.springer.de /papers/7321001/2300207/sc3.htm (1219 words)

	Roche lobe (Site not responding. Last check: 2007-10-26)
		It is approximately tear-drop shaped, withthe apex of the tear-drop pointing towards the other star (and the apex is at the Lagrange L1 point of the system).
		It is thisequipotential which defines the Roche lobes.
		This is not derivable from the Roche lobemodel as the coriolis force is a non- conservative force (i.e.not representable by a scalar potential).
	www.therfcc.org /roche-lobe-34737.html (229 words)

	Mass transfer - Wikipedia, the free encyclopedia
		The driving force for mass transfer is a difference in concentration; the random motion of molecules causes a net transfer of mass from an area of high concentration to an area of low concentration.
		In astronomy, mass transfer is the process by which matter gravitationally bound to a body, usually a star, fills its Roche lobe and becomes gravitationally bound to a second body, usually a compact object (white dwarf, neutron star or fl hole), and is eventually accreted onto it.
		It is a common phenomenon in binary systems, and may play an important role in some types of supernovae, and pulsars.
	en.wikipedia.org /wiki/Mass_transfer (225 words)

	Re: What are Roche lobes?
		This is because the Roche Lobe of a star is defined as the domain surrounding the star in which material released in co-rotation with the binary falls back on the star.
		Outside the Roche Lobe, material is either flung out of the system by "centrifugal forces," or falls on the companion star.
		The normal star is so close to the white dwarf that it is larger than its Roche Lobe, and is losing gas to the white dwarf, which forms a disk of gas orbiting the white dwarf.
	www.madsci.org /posts/archives/may98/895420780.As.r.html (375 words)

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