SPH models of an eccentric Be/X-ray binary show the disc never reaches steady state and neutron star accretion is strongest in near-coplanar prograde geometries, decreasing by orders of magnitude for misaligned retrograde orbits.
BRITEning up the Be Phenomenon
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abstract
Observations of 25 Ori much expand the picture derived of other early-type Be stars with BRITE and SMEI. Two instead of one difference frequencies rule the variability: (a) The lower one, 0.0129 c/d, is the frequency of events with full amplitudes of 100-200 mmag which may signal mass loss possibly driven by the higher one, 0.1777 c/d. (b) Much of the entire power spectrum is a tightly woven network of combination frequencies: (i) Below 0.25\,c/d, numerous frequencies are difference frequencies. (ii) Many frequencies above 2.5 c/d can be represented as sum frequencies and in a few cases as harmonics. (iii) Many frequencies between 1.1 and 1.75\,c/d can be portrayed as parents of combination frequencies. The number and fraction of combination frequencies increases steeply with decreasing amplitude and and accuracy of the frequency matching.
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Decretion disc evolution and neutron star accretion in short-period eccentric Be/X-ray binaries
SPH models of an eccentric Be/X-ray binary show the disc never reaches steady state and neutron star accretion is strongest in near-coplanar prograde geometries, decreasing by orders of magnitude for misaligned retrograde orbits.