Flare-Less Long Gamma-Ray Bursts and the Properties of Their Massive Progenitor Stars

Perna, Rosalba; MacFadyen, Andrew

doi:10.1088/2041-8205/710/2/l103

Cited by 10 publications

(8 citation statements)

References 43 publications

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“…As a final point, we may add that just as not all LGRBs exhibit this behavior, likewise it is clear from this work that not all progenitors are capable of producing the state transitions presented here. In fact, Perna & MacFadyen (2010) have recently argued that the lack of flaring activity in most LGRBs on long time scales is a signature of complete mixing in the progenitor, which is fully in agreement with the line of argument presented here. Once the deposition of energy in the inner regions of the star has produced a relativistic jet capable of traversing the stellar envelope, further variability may be reproduced in the overall light curve (Zhang et al 2003).…”

Section: Discussion and Prospects For Observabilitysupporting

confidence: 92%

Critical Angular Momentum Distributions in Collapsars: Quiescent Periods From Accretion State Transitions in Long Gamma-Ray Bursts

López-Cámara¹,

Lee²,

Ramírez-Ruiz³

2010

ApJ

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The rotation rate in pre-supernova cores is an important ingredient which can profoundly affect the post-collapse evolution and associated energy release in supernovae and long gamma ray bursts (LGRBs). Previous work has focused on whether the specific angular momentum is above or below the critical value required for the creation of a centrifugally supported disk around a black hole. Here, we explore the effect of the distribution of angular momentum with radius in the star, and show that qualitative transitions between high and low angular momentum flow, corresponding to high and low luminosity accretion states, can effectively be reflected in the energy output, leading to variability and the possibility of quiescent times in LGRBs.

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Section: Discussion and Prospects For Observabilitysupporting

confidence: 92%

Critical Angular Momentum Distributions in Collapsars: Quiescent Periods From Accretion State Transitions in Long Gamma-Ray Bursts

López-Cámara¹,

Lee²,

Ramírez-Ruiz³

2010

ApJ

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“…If this is not the case, then the nonmonotonicity (see, e.g., Heger et al 2000Heger et al , 2005Petrovic et al 2005) might have interesting consequences for the evolution of the accretion rate. For example, the accretion rate may surge if the average specific angular momentum in the shocked region drops below the critical value for rotational support near ISCO, and this might result in a "flaring" in the LGRB X-ray light curve (see, e.g., López-Cámara et al 2010;Perna & MacFadyen 2010).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Supernovae Powered by Collapsar Accretion in Gamma-Ray Burst Sources

Milosavljević¹,

Lindner

Shen

et al. 2011

ApJ

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The association of long-duration gamma-ray bursts (LGRBs) with Type Ic supernovae presents a challenge to supernova explosion models. In the collapsar model for LGRBs, gamma rays are produced in an ultrarelativistic jet launching from the magnetosphere of the black hole that forms in the aftermath of the collapse of a rotating progenitor star. The jet is collimated along the star's rotation axis, but the concomitant luminous supernova should be relatively-though certainly not entirely-spherical, and should synthesize a substantial mass of 56 Ni. Our goal is to provide a qualitative assessment of the possibility that accretion of the progenitor envelope onto the black hole, which powers the LGRB, could also deposit sufficient energy and nickel mass in the envelope to produce a luminous supernova. For this, the energy dissipated near the black hole during accretion must be transported outward, where it can drive a supernova-like shockwave. Here we suggest that the energy is transported by convection and develop an analytical toy model, relying on global mass and energy conservation, for the dynamics of stellar collapse. The model suggests that a ∼ 10, 000 km s −1 shock can be driven into the envelope and that ∼ 10 51 erg explosions are possible. The efficiency with which the accretion energy is being transferred to the envelope is governed by the competition of advection and convection at distances ∼ 100 − 1, 000 km from the black hole and is sensitive to the values of the convective mixing length, the magnitude of the effective viscous stress, and the specific angular momentum of the infalling envelope. Substantial masses of 56 Ni may be synthesized in the convective accretion flow over the course of tens of seconds from the initial circularization of the infalling envelope around the black hole. The synthesized nickel is convectively mixed with a much larger mass of unburned ejecta.

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“…Formation of the fallback disc ensue as material from the stellar envelope is thrown out at large distances during the supernova explosion; the fraction of this material which remains bound, falls back, and circularizes onto Keplerian orbits corresponding to their original specific angular momentum (Chevalier 1989;MacFadyen et al 2001; see also Perna & MacFadyen 2010 for an exploration of different angular momenta distributions in collapsing stars).…”

Section: Time Evolution Of the Accretion Flowmentioning

confidence: 99%

The influence of fallback discs on the spectral and timing properties of neutron stars

Yan

Perna

Soria

2012

Monthly Notices of the Royal Astronomical Society

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Fallback discs around neutron stars (NSs) are believed to be an expected outcome of supernova explosions. Here we investigate the consequences of such a common outcome for the timing and spectral properties of the associated NS population, using Monte Carlo population synthesis models. We find that the long‐term torque exerted by the fallback disc can substantially influence the late‐time period distribution, but with quantitative differences which depend on whether the initial spin distribution is dominated by slow or fast pulsars. For the latter, a single‐peaked initial spin distribution becomes bimodal at later times. Timing ages tend to underestimate the real age of older pulsars, and overestimate the age of younger ones. Braking indices cluster in the range 1.5 ≲n≲ 3 for slow‐born pulsars, and −0.5 ≲n≲ 5 for fast‐born pulsars, with the younger objects found predominantly below n≲ 3. Large values of n, while not common, are possible, and associated with torque transitions in the NS+disc system. The 0.1–10 keV thermal luminosity of the NS+disc system is found to be generally dominated by the disc emission at early times, yr, but this declines faster than the thermal surface emission of the NS. Depending on the initial parameters, there can be occasional periods in which some NSs switch from the propeller to the accretion phase, increasing their luminosity up to the Eddington limit for ∼103–104 years.

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Flare-Less Long Gamma-Ray Bursts and the Properties of Their Massive Progenitor Stars

Cited by 10 publications

References 43 publications

Critical Angular Momentum Distributions in Collapsars: Quiescent Periods From Accretion State Transitions in Long Gamma-Ray Bursts

Critical Angular Momentum Distributions in Collapsars: Quiescent Periods From Accretion State Transitions in Long Gamma-Ray Bursts

Supernovae Powered by Collapsar Accretion in Gamma-Ray Burst Sources

The influence of fallback discs on the spectral and timing properties of neutron stars

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