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Prog. Theor. Phys. Supplement No.143 (2001) pp. 50-77

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Jets and Central Engine of GRBs

Takashi Nakamura*

Yukawa Institute for Theoretical Physics, Kyoto University
Kyoto 606-8502, Japan

(Received April 27, 2001)

Abstract:

I argue various evidence for the physical association of GRB980425/SN1998bw. They are 1) the light curve and the line widths at late times, 2) the unusually low gamma ray luminosity of GRB980425 and the lack of high energy gamma rays, 3) the linear polarization of SN1998bw in the optical band, 4) the unusually slowly declining X-ray afterglow, 5) the peculiar spectral lag and the peak luminosity relation for GRB980425. In my picture GRB980425/SN1998bw is the collimated GRB observed with the viewing angle of ∼ 15° so that the X-ray afterglow should be slowly declining as observed ∼T-0.2. Even if GRB980425/SN1998bw is the only confirmed case of the association of GRB with supernova among ∼100 GRBs with accurate positions there is no serious statistical contradiction. If the viewing angle to the collimated GRB is small the afterglow is too bright and hides the supernova while if the viewing angle is too large GRB itself is too dim to be observed. From this it is estimated that SWIFT will detect ∼3GRB with supernova per year. The explosion energy of SN1998bw is ∼1052 erg and the total energy of GRB980425 is ∼1051 erg although the observed isotropic gamma ray energy is ∼1048 erg since we are observing the event from the side. This energy is just the rotational energy of the millisecond pulsar. I argue a possible evolutionary scenario of the binary stars leading to the formation of Type Ic supernova like SN1998bw and the millisecond magnetar which is the central engine of GRBs in my picture. Then the magnetar should exist in SN1998bw. If the soft gamma ray burst which is ten times larger than the famous March 5 event will occur in SN1998bw, it will be easy to detect the event. Next we argue the possible origin of X-ray precursors. We assume that internal shocks of GRBs consist of multiple sub-jets with a collimation half-angle ∼several×γi-1, where γi is the Lorentz factor of each sub-jet. If by chance a sub-jet is first emitted off-axis from the line of sight, the observed peak energy can be in the X-ray region. Next if by chance a subsequent sub-jet is emitted along the line of sight, then the peak energy will be in the gamma ray region and the gamma ray may arrive after the X-ray precursor from the former sub-jet depending on parameters. This model predicts a new class of GRBs with extremely weak gamma ray emission but X-ray precursor and/or postcursor. This new class might correspond to X-ray flashes or X-ray transients reported recently. (version 2001 April 27)


URL : http://ptp.ipap.jp/link?PTPS/143/50/
DOI : 10.1143/PTPS.143.50


*E-mail: takashi@yukawa.kyoto-u.ac.jp

[ Full Text PDF : FREE ACCESS (421K) ] Citation:

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