Accretion on to a binary from a polar circumbinary disc

We present hydrodynamical simulations to model the accretion flow from a polar circumbinary disc on to a high eccentricity (e = 0.78) binary star system with near unity mass ratio (q = 0.83), as a model for binary HD 98800 BaBb. We compare the polar circumbinary disc accretion flow with the previously studied coplanar case. In the coplanar case, the circumbinary disc becomes eccentric and the accretion alternates from being dominant on to one binary member to the other. For the polar disc case involving a highly eccentric binary, we find that the circumbinary disc retains its initially low eccentricity and that the primary star accretion rate is always about the same as the secondary star accretion rate. Recent observations of the binary HD 98800 BaBb, which has a polar circumbinary disc, have been used to determine the value of the H alpha flux from the brighter component. From this value, we infer that the accretion rate is much lower than for typical T Tauri stars. The eccentric orbit of the outer companion HD 98800 A increases the accretion rate on to HD 98800 B by similar to 20 per cent after each periastron passage. Our hydrodynamical simulations are unable to explain such a low accretion rate unless the disc viscosity parameter is very small, alpha < 10(-5). Additional observations of this system would be useful to check on this low accretion rate.

Automated summary

Hydrodynamical simulations have been used to model the accretion flow from a polar circumbinary disc onto a high eccentricity binary star system. The simulations show that the circumbinary disc retains its low eccentricity in the polar case, and the accretion rate on the primary star is similar to that on the secondary star. Recent observations of binary HD 98800 BaBb with a polar circumbinary disc suggest a lower accretion rate compared to typical T Tauri stars, possibly due to the eccentric orbit of the outer companion.