A rapidly spinning , strongly magnetized neutron star is invoked as the central engine for some Gamma-ray bursts ( GRBs ) , especially , the `` internal plateau " feature of X-ray afterglow .
However , for these `` internal plateau " GRBs , how to produce their prompt emission remains an open question .
Two different physical process have been proposed in the literature , ( 1 ) a new-born neutron star is surrounded by a hyper-accreting and neutrino cooling disk , the GRB jet can be powered by neutrino annihilation aligning the spin axis ; ( 2 ) a differentially rotating millisecond pulsar was formed due to different angular velocity between the interior core and outer shell parts of the neutron star , which can power an episodic GRB jet .
In this paper , by analyzing the data of one peculiar GRB 070110 ( with internal plateau ) , we try to test which model being favored .
By deriving the physical parameters of magnetar with observational data , the parameter regime for initial period ( P _ { 0 } ) and surface polar cap magnetic field ( B _ { p } ) of the central NS are ( 0.96 \sim 1.2 ) ~ { } ms and ( 2.4 \sim 3.7 ) \times 10 ^ { 14 } ~ { } G , respectively .
The radiative efficiency of prompt emission is about \eta _ { \gamma } \sim 6 \% .
However , the radiative efficiency of internal plateau ( \eta _ { X } ) is larger than 31 \% assuming the M _ { NS } \sim 1.4 M _ { \odot } and P _ { 0 } \sim 1.2 ~ { } ms .
The clear difference between the radiation efficiencies of prompt emission and internal plateau implies that they maybe originated from different components ( e.g .
prompt emission from the relativistic jet powered by neutrino annihilation , while the internal plateau from the magnetic outflow wind ) .