ay45c4-page45 - Referring to the gure in 4.3.4, you can see...

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Unformatted text preview: Referring to the gure in 4.3.4, you can see that jrL1 rCoMj can be significantly less than r (the 2-body separation). A consequence is that gas that ows over L1 has only enough angular momentum to go into a circular orbit well inside the other Roche lobe | if it does not impact the surface of the other star rst. If the other star is a white dwarf or neutron star, so-called \compact objects," it is small enough to allow the formation of an \accretion disk" of gas (see gure). Once in the accretion disk, gas slowly spirals into the compact object by the action of viscous forces (including magnetic and turbulent viscosity). Ω "Normal star" Disk DDsk L1 4.3.7 The Lagrange points Referring again to the contour plot in 4.3.4, let us now take the masses to be safely tucked for inside their Roche lobes, as for the Earth and Moon, or Sun and Jupiter. We now ask the question: Are there any equilibrium points where a third orbiting test body could be placed, and where it would 104 ...
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