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A rapidly spinning, strongly magnetized neutron star is invoked as thecentral engine for some Gamma-ray bursts (GRBs), especially, the $"$internalplateau$"$ feature of X-ray afterglow. However, for these $"$internalplateau$"$ GRBs, how to produce their prompt emission remains an open question.Two different physical process have been proposed in the literature, (1) anew-born neutron star is surrounded by a hyper-accreting and neutrino coolingdisk, the GRB jet can be powered by neutrino annihilation aligning the spinaxis; (2) a differentially rotating millisecond pulsar was formed due todifferent angular velocity between the interior core and outer shell parts ofthe neutron star, which can power an episodic GRB jet. In this paper, byanalyzing the data of one peculiar GRB 070110 (with internal plateau), we tryto test which model being favored. By deriving the physical parameters ofmagnetar with observational data, the parameter regime for initial period($P_{0\rm }$) and surface polar cap magnetic field ($B_{\rm p}$) of the centralNS are $(0.96\sim 1.2 )~\rm ms$ and $(2.4\sim 3.7)\times 10^{14}~\rm G$,respectively. The radiative efficiency of prompt emission is about$\eta_{\gamma} \sim 6\%$. However, the radiative efficiency of internal plateau($\eta_{\rm X}$) is larger than $31\%$ assuming the $M_{\rm NS}\sim1.4M_{\odot}$ and $P_{0\rm }\sim1.2 ~\rm ms$. The clear difference between theradiation efficiencies of prompt emission and internal plateau implies thatthey maybe originated from different components (e.g. prompt emission from therelativistic jet powered by neutrino annihilation, while the internal plateaufrom the magnetic outflow wind).

The radiative efficiency of relativistic jet and wind: A case study of GRB 070110