The most likely origin of hypervelocity stars ( HVSs ) 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 _ { \odot } B-type main-sequence star moving with a heliocentric radial velocity of about 720 km s ^ { -1 } at a distance of \sim 60 { kpc } , and the recent discovered hypervelocity binary candidate ( HVB ) , traveling at \sim 570 km s ^ { -1 } , challenge this standard scenario . Recently , Fragione & Gualandris ( 2018 ) 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 center of mass ( the so-called 2+2 quadruples ) are \approx 4 \% of the stars in the solar neighborhood . 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 \lesssim 2 - 4 \% , which translates into an ejection rate of \lesssim 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 .