When the matter from a companion star is accreted towards the central compact accretor , i.e .
a black hole ( BH ) or a neutron star ( NS ) , an accretion disc and a jet outflow will form , providing bight X-ray and radio emission , which is known as X-ray binaries ( XRBs ) .
In the low/hard state , there exist disc-jet couplings in XRBs , but it remains uncertain whether the jet power comes from the disc or the central accretor .
Moreover , BHXRBs have different properties compared with NSXRBs : quiescent BHXRBs are typically two to three orders of magnitude less luminous than NSXRBs in X-ray , whereas BHXRBs are more radio loud than NSXRBs .
In observations , an empirical correlation has been established between radio and X-ray luminosity , L _ { R } \propto L _ { X } ^ { b } , where b \sim 0.7 for BHXRBs and b \sim 1.4 for non-pulsating NSXRBs .
However , there are some outliers of BHXRBs showing unusually steep correlation as NSXRBs at higher luminosities .
In this work , under the assumption that the origin of jet power is related to the internal energy of the inner disc , we apply our magnetized , radiatively efficient thin disc model and the well-known radiatively inefficient accretion flow model to NSXRBs and BHXRBs .
We find that the observed radio/X-ray correlations in XRBs can be well understood by the disc-jet couplings .