Physics
Scientific paper
Nov 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998pthph.100..921n&link_type=abstract
Progress of Theoretical Physics, Vol. 100, No. 5, pp. 921-929.
Physics
42
Scientific paper
As a progenitor of NHE (Non High Energy) GRBs (Gamma Ray Bursts), we propose a (C + O) star and a neutron star (black hole) close binary system with separation ~ 0.2 Rodot. Since the (C + O) star is tidally locked, the collapsing core should have a spin angular momentum ~ 6 × 1048 cgs, so that a new-born pulsar should be a milli-second pulsar (MSP) (P ~ 1 ms). An α - Ω dynamo in the first 10 s after the bounce of the core will generate a super strong magnetic field (B ~ 1016 G). The beam of energy from a super strongly magnetized milli-second pulsar (SSM-MSP) can punch a hole in the supernova ejecta . Then the beam of gamma rays flows out of the ejecta for ~ 10 s with a total energy up to ~ 2 × 1051 erg. If we observe this beam from the lateral direction, the energy of gamma rays should be smaller than 500 keV due to the electron scattering and the total energy of gamma rays should be much smaller than ~ 2 × 1051 erg, which are the very characteristics of NHE-GRBs. In the SSM-MSP model of NHE-GRB, GRB events should be associated with Type Ib/Ic supernova, like GRB980425/SN1998bw. If a SSM-MSP is produced in a fraction (~ a few %) of Type Ib/Ic supernovae, the event rate as well as the isotropic and homogeneous distribution of NHE-GRBs can also be explained. According to this model a pulsar with a spin period P ~ 1.4 s (B/1016) (t/4 month)1/2 should exist in SN1998bw, so that the search for this pulsar in all the wave length is urgent. SSM-MSPs can accelerate protons up to ~ 3 × 1022 (P/1 ms)-2 (B/1016 G)eV. If a few % (~ 1050 erg) of the beam energy of SSM-MSP in NHE-GRB event (> 5 × 1051 erg) is in the form of high energy protons of energy ~ 1020 eV, the flux of the observed UHECRs (Ultra High Energy Cosmic Rays) can be explained. Then it should be possible to find a supernova remnant along the direction of each UHECR. As a natural implication of our model, it is suggested that a NHE-GRB is a part of the progenitor of a soft gamma ray repeater which also has a superstrong magnetic field (B ~ 1015 G) and is in a supernova remnant.
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