Magnetized relativistic jets and long-duration GRBs from magnetar spin-down during core-collapse supernovae

By N. Bucciantini, E. Quataert, B. Metzger, T. Thompson, J. Arons, L. Berkeley, Ohio state Univ., U. Firenze. 2009

143 citations recorded by the source corpus.

We use ideal axisymmetric relativistic magnetohydrodynamic simulations to calculate the spin-down of a newly formed millisecond, B ∼ 10 15 G, magnetar and its interaction with the surrounding stellar envelope during a core-collapse supernova (SN) explosion. The mass, angular momentum and rotational energy lost by the neutron star are determined self-consistently given the thermal properties of the cooling neutron star's atmosphere and the wind's interaction with the surrounding star. The magnetar drives a relativistic magnetized wind into a cavity created by the outgoing SN shock. For high spin-down powers (∼10 51 ―10 52 erg s ―1 ), the magnetar wind is superfast at almost all latitudes, while for lower spin-down powers (∼10 50 erg s ―1 ), the wind is subfast but still super-Alfvenic. In all cases, the rates at which the neutron star loses mass, angular momentum and energy are very similar to the corresponding free wind values (≤30 per cent differences), in spite of the causal contact between the neutron star and the stellar envelope. In addition, in all cases that we consider, the magnetar drives a collimated (∼5―10°) relativistic jet out along the rotation axis of the star. Nearly all of the spin-down power of the neutron star escapes via this polar jet, rather than being transferred to the more spherical SN explosion. The properties of this relativistic jet and its expected late-time evolution in the magnetar model are broadly consistent with observations of long duration gamma-ray bursts (GRBs) and their associated broad-lined Type Ic SN.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c383ba8dcff861aeb9850669375d450f2779884f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation (2015, background): “This choice corresponds to the assumption of a large-scale magnetic flux threading the progenitor star (Bucciantini et al. 2009).”
Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation (2011, methodology): “…where the magnetization in the wind evolves according to the value near the light cylinder predicted from evolutionary models including PNS cooling (Bucciantini et al. 2009); and (2) because a variety of processes at work in the wind, the termination shock, and the nebula, may dissipate the…”
The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “As toroidal flux accumulates in the nebula, magnetic forces – and the anisotropic thermal pressure they induce – redirect the equatorial outflow towards the poles (Begelman & Li 1992; Königl & Granot 2002; Uzdensky & MacFadyen 2007; Bucciantini et al. 2007, 2008, 2009; Komissarov & Barkov 2007).”
A POSSIBLE CONNECTION BETWEEN FAST RADIO BURSTS AND GAMMA-RAY BURSTS (2013, background): “If one accepts that a millisecond magnetar is indeed operating in both long (Usov 1992; Bucciantini et al. 2009; Metzger et al. 2011) and short (Dai et al. 2006; Fan & Xu 2006; Metzger et al. 2008; Kiuchi et al. 2012) GRBs1, then the very steep decay at the end of internal plateaus suggests that…”
BRIGHT SUPERNOVAE FROM MAGNETAR BIRTH (2009, background): “On the one hand, this might facilitate the magnetar paradigm because the production of the necessary large amount of 56Ni has proven problematic (Bucciantini et al. 2009).”
The physics of gamma-ray bursts & relativistic jets (2014, background): “…Nagataki, 2009, 2011), and a rapidly spinning, highly magnetized, neutron star or “fast magnetar” (Usov, 1992; Thompson, 1994; Dai and Lu, 1998a; Kluźniak and Ruderman, 1998; Wheeler et al., 2000; Zhang and Mészáros, 2001a; Dai et al., 2006; Bucciantini et al., 2008, 2009; Metzger et al., 2011).”
On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, background): “However, the required magnetar parameters in GRB models are more extreme than for SLSNe, with spin periods ∼1 ms and magnetic fields 10–100 times stronger, in order to drive a jet that punches through the stellar envelope (Bucciantini et al. 2009).”
The diversity of transients from magnetar birth in core collapse supernovae (2015, background): “This collimation may be facilitated by the anisotropic stress induced by the strong toroidal magnetic field in the nebula separating the magnetar wind from the surrounding star (Bucciantini et al. 2009).”
SUPERNOVA LIGHT CURVES POWERED BY YOUNG MAGNETARS (2009, background): “…may also be sources for ultra-high energy cosmic rays (Arons 2003) or deposit enough energy in the collapsing stellar envelope to favorably shape the deep interior (Uzdensky & MacFadyen 2007; Bucciantini et al. 2009) for the production of a collimated relativistic flow needed for gamma-ray bursts.”
A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, background): “…winds have been extensively explored previously in the context of gamma-ray bursts from core collapse supernovae (Thompson et al. 2004; Bucciantini et al. 2006, 2007, 2008, 2009; Metzger et al. 2007, 2008c, 2011; Vlasov et al. 2014, 2017) and NS mergers (Metzger et al. 2008b;…”
The unusual X-ray emission of the short Swift GRB 090515: evidence for the formation of a magnetar? (2010, background): “Simulations have shown that a relativistic jet can be produced by a magnetar (Bucciantini et al. 2009).”
SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL (2013, methodology): “This is a major limitation of using the homologous expansion approximation, and the consequences for the light curve can only be investigated with numerical radiation hydrodynamics (see Bucciantini et al. 2009, and reference therein for some examples).”