The late time evolution of gamma-ray bursts: ending hyperaccretion and producing flares

By D. Proga, Bing Zhang. 2006

155 citations recorded by the source corpus.

We consider the properties of a hyperaccretion model for gamma-ray bursts (GRBs) at late times when the mass supply rate is expected to decrease with time. We point out that the region in the vicinity of the accretor and the accretor itself can play an important role in determining the rate of accretion, and its time behaviour, and ultimately the energy output. Motivated by numerical simulations and theoretical results, we conjecture that the energy release can be repeatedly stopped and then restarted by the magnetic flux accumulated around the accretor. We propose that the episode or episodes when the accretion resumes correspond to X-ray flares discovered recently in a number of GRBs.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9f886acb64789a2196086544fad5efe89e323041

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. B. Metzger
4. Ramesh Narayan
5. E. Berger
6. A. Tchekhovskoy
7. E. Liang
8. E. Quataert

Citations in the corpus

• The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, background): “…the engine and/or late internal shocks (Fan & Wei 2005; Burrows et al. 2005; Wu et al. c© 2005 RAS, MNRAS 000, 1–15 The Ep,i – Eiso correlation in GRBs: update, re–analysis and main implications 11 2006; Perna et al. 2006; Proga & Zhang 2006) and thus can be considered part of the prompt emission.”
• Efficient Generation of Jets from Magnetically Arrested Accretion on a Rapidly Spinning Black Hole (2011, background): “The quasi-periodic nature of the fluctuations in η suggests magnetically arrested accretion as a possible mechanism to produce low-frequency QPOs in accreting stellar-mass BHs (Remillard & McClintock 2006) and variability in AGN (Ghisellini et al. 2010) and GRB outflows (Proga & Zhang 2006).”
• Short-Duration Gamma-Ray Bursts (2013, background): “Proga & Zhang (2006) suggest that the accretion can be episodically stopped and re-started through variations in the accumulated magnetic flux around the accreting central engine.”
• Time-dependent models of accretion discs formed from compact object mergers (2008, background): “…to a number of different sources, including fragmentation of a rapidly rotating core (King et al. 2005), magnetic regulation of the accretion flow (Proga & Zhang 2006), fragmentation of the accretion disk (Perna et al. 2005; although this explanation may have difficulty reproducing the observed…”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “• Proga and Zhang [749] argued that accumulation of magnetic flux near the black hole during accretion can temporarily build up a ‘‘magnetic barrier’’, which shuts down accretion for some time.”
• Gamma-ray burst afterglows (2006, methodology): “Based on the MHD numerical simulations in other contexts and theoretical arguments , Proga & Zhang (2006) argue that the magnetic barrier near the black hole may act as an effective modulator of the accretion flow.”
• General relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around black holes (2012, background): “For example, the suspended inflow seen in 2D axisymmetric MHD simulations (McKinney & Gammie 2004; Proga & Zhang 2006; Komissarov & Barkov 2009) is due to axisymmetry (Igumenshchev 2008, 2009).”
• FORMATION OF STABLE MAGNETARS FROM BINARY NEUTRON STAR MERGERS (2013, background): “…hard to explain if all the BNS mergers produce an HMNS which collapses to a BH in less than ∼ 1s; the remnant torus is also expected to be completely accreted on the same timescale (Rezzolla et al. 2011), unless magnetic or gravitational instabilities set in (Proga & Zhang 2006; Perna et al. 2006).”
• Making a Short Gamma-Ray Burst from a Long One: Implications for the Nature of GRB 060614 (2006, background): “Alternatively, disk fragmentation (Perna et al. 2006) or magnetic field barrier near the accretor (Proga & Zhang 2006) would induce intermittent accretion that power the flares.”
• Gamma-Ray Bursts in the Swift Era (2009, background): “…the flow patterns near relativistic objects accreting matter in the hypercritical regime (Di Matteo et al. 2002, Chen and Beloborodov 2007, Proga and Zhang 2006, Perna et al. 2006, Shibata et al. 2007, Kumar et al. 2008), where photons are unable to provide cooling but neutrinos do so…”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “The progenitor and central engine models must then be modified to invoke a much longer accretion time scale (King et al. 2005; Perna et al. 2006; Proga & Zhang 2006), or a non-BH-torus central engine (Dai et al. 2006; Staff et al. 2007).”
• Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, background): “A final possibility is that a strong magnetic flux may accumulate around the black hole during the accretion and may then repeatedly stop and restart the accretion, causing flares in the X-ray omission (Proga & Zhang 2006).”
• Gamma-Ray Bursts in the Swift Era (2007, background): “Based on MHD numerical simulations in other contexts (e.g. Proga & Begelman 2003) and theoretical arguments, Proga & Zhang (2006) argued that a magnetic barrier near the black hole may act as an effective modulatorof the accretion flow.”
• Unveiling the origin of X-ray flares in gamma-ray bursts (2010, background): “As discussed in the literature (Proga & Begelman 2003; King et al. 2005; Perna et al. 2006; Proga & Zhang 2006; Kumar et al. 2008; Lopez-Camara et al. 2009), there are several mechanisms that could keep the central engine active for a long time or reactivate it in a pseudo-random way.”
• Swift Observations of GRB 070110: An Extraordinary X-Ray Afterglow Powered by the Central Engine (2007, background): “…X-ray flares therefore require that the central engine accretes episodically, either due to fragmentation or density fluctuation of the accretion disc (e.g. King et al. 2005; Perna et al. 2006; Rosswog 2006), or due to modulation of the magnetic fields near the accretor (Proga & Zhang 2006).”