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One favored progenitor model for short duration gamma-ray bursts (SGRBs) isthe coalescence of two neutron stars (NS-NS). One possible outcome of such amerger would be a rapidly spinning, strongly magnetized neutron star (known asa millisecond magnetar). These magnetars may be "supra-massive", implying theywould collapse to black holes after losing centrifugal support due to magneticdipole spindown. By systematically analyzing the BAT-XRT light curves of allshort GRBs detected by {\em swift}, we test how well the data are consistentwith this central engine model of short GRBs. We find that the so-called"extended emission" observed with BAT in some short GRBs are fundamentally thesame component as the "internal X-ray plateau" as observed in many short GRBs,which is defined as a plateau in the lightcurve followed by a very rapid drop.Based on how likely a short GRB hosts a magnetar, we characterize the entire{\em Swift} short GRB sample into three categories: the "internal plateau"sample, the "external plateau" sample, and the "no plateau" sample. The derivedmagnetar surface magnetic field $B_{\rm p}$ and the initial spin period $P_0$fall into the reasonable range. No GRBs in the internal plateau sample have thetotal energy exceeding the maximum energy budget of a millisecond magnetar.Assuming that the rapid fall time at the end of the internal plateau is thecollapse time of a supra-massive magnetar to a black hole, and applying themeasured mass distribution of NS-NS systems in our Galaxy, we constrain theneutron star equation of state (EOS). The data suggest that the NS equation ofstate is close to the GM1 model, which has a maximum non-rotating NS mass$M_{\rm TOV} \sim 2.37 M_\odot$.

The Millisecond Magnetar Central Engine in short GRBs