Growth and Dissipation of Be Star Discs in Misaligned Binary Systems
| Autor: | M. W. Suffak, Carol E. Jones, Alex C. Carciofi |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Physics
010308 nuclear & particles physics Be star media_common.quotation_subject FOS: Physical sciences Astronomy and Astrophysics Astrophysics Radius Dissipation Orbital period 01 natural sciences Orbit Circular motion Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science 0103 physical sciences Precession Astrophysics::Earth and Planetary Astrophysics Eccentricity (behavior) 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics media_common |
| Popis: | We use a three-dimensional smoothed particle hydrodynamics code to simulate growth and dissipation of Be star discs in systems where the binary orbit is misaligned with respect to the spin axis of the primary star. We investigate six different scenarios of varying orbital period and misalignment angle, feeding the disc at a constant rate for 100 orbital periods, and then letting the disc dissipate for 100 orbital periods. During the disc growth phase, we find that the binary companion tilts the disc away from its initial plane at the equator of the primary star before settling to a constant orientation after 40 to 50 orbital periods. While the mass-injection into the disc is ongoing, the tilting of the disc can cause material to reaccrete onto the primary star prematurely. Once disc dissipation begins, usually the disc precesses about the binary companion's orbital axis with precession periods ranging from 20 to 50 orbital periods. In special cases we detect phenomena of disc tearing, as well as Kozai-Lidov oscillations of the disc. These oscillations reach a maximum eccentricity of about 0.6, and a minimum inclination of about \ang{20} with respect to the binary's orbit. We also find the disc material to have highly eccentric orbits beyond the transition radius, where the disc changes from being dominated by viscous forces, to heavily controlled by the companion star, in contrast to its nearly circular motion inward of the transition radius. Finally, we offer predictions to how these changes will affect Be star observables. 14 pages, 14 figures |
| Databáze: | OpenAIRE |
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