Abstract
We compare Smoothed Particle Hydrodynamic simulations of retrogradely precessing accretion disks that have a white dwarf primary and a main sequence secondary with observational data and with theory on retrograde precession via tidal torques like those by the Moon and the Sun on the Earth (1, 2). Assuming the primary does not accrete much of the mass lost from the secondary, we identify the theoretical low mass star/brown dwarf boundary. We find no observational candidates in our study that could qualify as brown dwarfs.
Highlights
Politano & Weisler [3] find that 75% of simulated zero-age Cataclysmic Variables (ZACVs) forming with Brown Dwarfs (BDs) had, once-upon-a-time, solar-type progenitor primaries in binaries with orbital separations less than 3 A.U
A second formation of CVs with BDs is when a low-mass secondary has lost enough mass to the white dwarf (WD) via accretion that its mass has dropped below the hydrogen-burning limit
EPJ Web of Conferences presented in Montgomery [1] that is based on the retrograde precession of Earth via tidal torques by the Moon and the Sun
Summary
Politano & Weisler [3] find that 75% of simulated zero-age Cataclysmic Variables (ZACVs) forming with Brown Dwarfs (BDs) had, once-upon-a-time, solar-type progenitor primaries in binaries with orbital separations less than 3 A.U. We compare Smoothed Particle Hydrodynamic simulations of retrogradely precessing accretion disks that have a white dwarf primary and a main sequence secondary with observational data and with theory on retrograde precession via tidal torques like those by the Moon and the Sun on the Earth [1, 2]. Assuming the primary does not accrete much of the mass lost from the secondary, we identify the theoretical low mass star/brown dwarf boundary.
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