2018MNRAS.479.2615F

The most likely origin of hypervelocity stars is the tidal disruption of a binary star by the supermassive black hole (MBH) in the Galactic Centre (GC). However, HE0437-5439, a 9 M_☉B-type main-sequence star moving with a heliocentric radial velocity of about 720 kms^–1 at a distance of ∼60 kpc, and the recent discovered hypervelocity binary candidate (HVB), travelling at ∼570 kms^–1, challenge this standard scenario. Recently, Fragione & Gualandris have demonstrated that the tidal breakup of a triple star leads to an insufficient rate. Observations show that quadruple stars made up of two binaries orbiting their common centre of mass (the so-called 2+2 quadruples) are ~4 percent of the stars in the solar neighbourhood. Although rarer than triples, 2+2 quadruple stars may have a role in ejecting HVBs as due to their larger energy reservoir. We present a numerical study of 2+2 quadruple disruptions by the MBH in the GC and find that the production of HVBs has a probability ≲2-4 percent, which translates into an ejection rate of ≲1 Gyr^–1, comparable to the triple disruption scenario. Given the low-ejection rate, we suggest that alternative mechanisms are responsible for the origin of HVBs, as the ejection from the interaction of a young star cluster with the MBH in the GC and the origin in the Large Magellanic Cloud.