2024/04/27 by Rebecca G. Martin, Martin, Rebecca G., Stephen H. Lubow +5
Earth and Planetary Sciences · Physics and Astronomy · #Advanced X-ray Imaging Techniques #Astrophysical Phenomena and Observations #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #High-pressure geophysics and materials
paper · pdf · doi:10.48550/arxiv.2404.17976
openalex publication_date 2024/04/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
With three-dimensional hydrodynamical simulations we show that the size of the decretion disc and the structure of the accretion flow onto the neutron star in a Be/X-ray binary strongly depends upon the disc aspect ratio, H/R. We simulate a Be star disc that is coplanar to the orbit of a circularly or moderately eccentric neutron star companion, thereby maximising the effects of tidal truncation. For low disc aspect ratio, H/R\lesssim 0.1, the disc is efficiently tidally truncated by the neutron star. Most material that escapes the Roche lobe of the Be star is accreted by the neutron star through tidal streams. For larger disc aspect ratio, the outflow rate through the Be star disc is higher, tidal truncation becomes inefficient, the disc fills the Roche lobe and extends to the orbit of the companion. Some material escapes the binary as a gas stream that begins near the L2 point. While the accretion rate onto the neutron star is higher, the fraction of the outflow that is accreted by the neutron star is smaller. Low density Be star discs are expected to be approximately isothermal, such that H/R increases with radius. Tidal truncation is therefore weaker for larger separation binaries, and lower mass primaries.