Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation
By N. Bucciantini, B. Metzger, T. Thompson, E. Quataert. 2011
167 citations recorded by the source corpus.
Approximately 1/4-1/2 of short duration Gamma-Ray Bursts are followed by variable X-ray emission lasting ~ 100 s with a fluence comparable or exceeding that of the initial burst itself. The long duration and significant energy of this `extended emission'(EE) poses a major challenge to the standard binary neutron star merger model. metzger08 recently proposed that the EE is powered by the spin-down of a strongly magnetized neutron star. However, the effects of surrounding material on the magnetar outflow have not yet been considered. Here we present time-dependent axisymmetric relativistic magnetohydrodynamic simulations of the interaction of the relativistic proto-magnetar wind with a surrounding 10^-1 10^-3 M_\odot envelope, which represents material ejected during the merger; the supernova following AIC; or via outflows from the accretion disk. The collision between the relativistic magnetar wind and the expanding ejecta produces a magnetized nebula inside the ejecta. A strong toroidal magnetic field builds up in the nebula, which drives a bipolar jet out through the ejecta, similar to the magnetar model developed in the case of long duration GRBs. We quantify the `break-out' time and opening angle of the jet theta_j as a function of the wind energy flux dot{E} and ejecta mass M_ej. We show that dot{E} and theta_j are inversely correlated, such that the beaming-corrected (isotropic) luminosity of the jet is primarily a function of M_ej. Both variability arguments, and the lower limit on the power of magnetar outflows capable of producing bright emission, suggest that the true opening angle of the magnetar jet must be relatively large. The model thus predicts a class of events for which the EE is observable with no associated short GRB. These may appear as long-duration GRBs or X-Ray Flashes, which may be detected by future all-sky X-ray survey missions.
Subfields: Astronomy and Astrophysics, Atmospheric Science
View Paper: https://www.semanticscholar.org/paper/8b4f30f2dc8ec4ebac042fb697a93b24cee282f8
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Citations in the corpus
- Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, background): “This makes it more likely that a massive NS remnant could remain (e.g.,̈Ozel et al. 2010; Bucciantini et al. 2012; Giacomazzo & Perna 2013; Kiziltan et al. 2013).”
- Kilonova light curves from the disc wind outflows of compact object mergers (2014, background): “GRB 080503 was accompanied by extremely bright extended prompt X-ray emission, which Metzger et al. (2008a) speculate is powered by a stable magnetar created during an NS–NS merger (see also Bucciantini et al. 2012; Ciolfi & Siegel 2015, Rezzolla & Kumar 2015).”
- The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts (2014, methodology): “Both features are difficult to explain through, for example, fall-back accretion on to black hole central engines (Metzger et al. 2008; Bucciantini et al. 2012, and references therein), although see Siegel, Ciolfi & Rezzolla (2014).”
- WHAT IS THE MOST PROMISING ELECTROMAGNETIC COUNTERPART OF A NEUTRON STAR BINARY MERGER? (2011, background): “Although the origin of this extended emission is still debated, one explanation is that it results from ongoing energy output from a highly magnetized neutron star, which survives the NS-NS merger (Metzger et al. 2008b; Bucciantini et al. 2011).”
- Signatures of magnetar central engines in short GRB light curves (2013, background): “Additionally, this region is defined using angular momentum conservation during the AIC of a WD (Usov 1992) and is not a physically forbidden region.”