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• W2799034047 abstract "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." @default.
• W2799034047 created "2018-05-07" @default.
• W2799034047 creator A5079113338 @default.
• W2799034047 date "2018-06-14" @default.
• W2799034047 modified "2023-10-18" @default.
• W2799034047 title "Tidal breakup of quadruple stars in the Galactic Centre" @default.
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• W2799034047 doi "https://doi.org/10.1093/mnras/sty1593" @default.
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