In recent years several hypervelocity stars ( HVSs ) have been observed in the halo of our Galaxy .
Such stars are thought to be ejected through dynamical interactions near the massive black hole ( MBH ) in the Galactic center .
Three scenarios have been suggested for their ejection ; binary disruption by a MBH , scattering by inspiraling IMBH and scattering by stellar BHs close to MBH .
These scenarios involve different stellar populations in the Galactic center .
Here we use observations of the Galactic center stellar population together with dynamical and evolutionary arguments to obtain strong constraints on the nature and origin of HVSs .
We show that the IMBH inspiral scenario requires too many ( \mathcal { O } ( 10 ^ { 3 } ) main sequence B stars to exist close to the MBH ( < 0.01 pc ) at the time of inspiral , where current observations show \mathcal { O } ( 10 ) such stars .
Scattering by SBHs also require too many B stars to be observed in the GC , but it may contribute a small fraction of the currently observed HVSs .
The binary disruption scenario is still consistent with current observations .
In addition it is shown that recently suggested signatures for HVSs origin such as hypervelocity binaries and slow rotating HVSs are much weaker than suggested and require too large statistics .
In addition , we show that due to the conditions close to the MBH most binary star systems are not expected to survive for long in this region .
Consequently , unique stellar populations that require long evolution in binaries are not expected to be ejected as HVSs in the BHs scattering mechanisms ( this may also be related to to the recently observed asymmetry in the velocity distribution of HVSs ) .