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Estimating the space density of ultracompact binary stars

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Figure

Figure 1.1: Equipotential surfaces of the Roche geometry for a binary with a massratio, q=0.2
Figure 1.2: Schematic representation of the common envelope phase. The core of theevolved star (black dot in the larger Roche lobe) and the less massive main sequencestar (large filled circle in the smaller lobe) orbit around the centre of mass of the syste
Figure 1.3: Schematic view of magnetic braking in close binary systems.Ionisedparticles are forced to flow along the magnetic field lines, before being released at largedistances from the star, carrying away angular momentum
Figure 1.4: Illustration showing the formation of an accretion disc via Roche lobeoverflow
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