Understanding the engines and progenitors of gamma-ray bursts

Fryer, Chris L.; Lloyd-Ronning, Nicole M.; Wollaeger, Ryan; Wiggins, Brandon; Miller, Jonah; Dolence, Joshua C.; Ryan, Ben; Fields, Carl

doi:10.1140/epja/i2019-12818-y

Cited by 31 publications

(39 citation statements)

References 109 publications

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“…Although the requirement for a stripped envelope progenitor with a large reserve of angular momentum at corecollapse is understood, the exact nature of the progenitors and the evolutionary pathways which lead to long-duration (core-collapse) GRBs are not well constrained (see Levan et al 2016;Fryer et al 2019, and others for reviews). Models invoking single stars struggle to maintain enough angular momentum over the stellar lifetime, while simultaneously losing the outer envelope through winds (Vink et al 2001;Hirschi et al 2005;Vink & de Koter 2005;Woosley & Bloom 2006;Vink et al 2011;Modjaz et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Chrimes

Stanway

Eldridge

2019

Monthly Notices of the Royal Astronomical Society

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Long-duration gamma-ray bursts (GRBs) are understood to be the final fate for a subset of massive, stripped envelope, rapidly rotating stars. Beyond this, our knowledge of the progenitor systems is limited. Using the BPASS (Binary Population and Spectral Synthesis) stellar evolution models, we investigate the possibility that some massive stars in binaries can maintain the angular momentum required for jet production, while still loosing their outer envelope through winds or binary interactions. We find that a total hydrogen mass of M H < 5 × 10 −4 M and a helium ejecta mass fraction of F He < 0.20 provide the best thresholds for the supernova II/Ibc and Ib/Ic divisions respectively. Tidal interactions in binaries are accounted for by applying a tidal algorithm to post-process the stellar evolution models output by BPASS. We show that the observed volumetric gamma-ray burst rate evolution can be recreated using two distinct pathways and plausible distributions for burst parameters. In the first pathway, stars are spun up by mass accretion into a quasi-homogeneous state. In the second, tides maintain rotation where otherwise the star would spin down. Both lead to type Ic supernova progenitors, and a metallicity distribution consistent with the GRB host galaxy population. The inferred core angular momentum threshold for jet production is consistent with theoretical requirements for collapsars, given the assumptions made in our model. We can therefore reproduce several aspects of core collapse supernova/GRB observation and theory simultaneously. We discuss the predicted observable properties of GRB progenitors and their surviving companions.

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Section: Introductionmentioning

confidence: 99%

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Chrimes

Stanway

Eldridge

2019

Monthly Notices of the Royal Astronomical Society

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“…Many models propose ways in which this central engine may be formed (e.g. see Fryer et al 2019, and references therein), but the exact mechanism is still unknown.…”

Section: Determining Source Size and Geometrymentioning

confidence: 99%

Constraining properties of neutron star merger outflows with radio observations

Dobie

Kaplan

Hotokezaka

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The jet opening angle and inclination of GW170817 -the first detected binary neutron star merger -were vital to understand its energetics, relation to short gamma-ray bursts, and refinement of the standard siren-based determination of the Hubble constant, H 0 . These basic quantities were determined through a combination of the radio lightcurve and Very Long Baseline Interferometry (VLBI) measurements of proper motion. In this paper we discuss and quantify the prospects for the use of radio VLBI observations and observations of scintillation-induced variability to measure the source size and proper motion of merger afterglows, and thereby infer properties of the merger including inclination angle, opening angle and energetics. We show that these techniques are complementary as they probe different parts of the circum-merger density/inclination angle parameter space and different periods of the temporal evolution of the afterglow. We also find that while VLBI observations will be limited to the very closest events it will be possible to detect scintillation for a large fraction of events beyond the range of current gravitational wave detectors. Scintillation will also be detectable with next generation telescopes such as the Square Kilometre Array, 2000 antenna Deep Synoptic Array and the next generation Very Large Array, for a large fraction of events detected with third generation gravitational wave detectors. Finally, we discuss prospects for the measurement of the H 0 with VLBI observations of neutron star mergers and compare this technique to other standard siren methods.

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“…It can be even more difficult to tie GRBs to specific massive stars. The black-hole accretion disk (BHAD) paradigm (Popham et al 1999;Fryer et al 1999) for GRBs has both fit existing data and made observational predictions that have been subsequently confirmed (for a review, see Fryer et al 2019). In this paper, we focus on Type I Collapsars, those formed from the so-called direct-collapse scenario of black hole formation (Heger et al 2003) where the black hole forms without launching a supernova explosion.…”

Section: Introductionmentioning

confidence: 87%

“…As we shall see in our comparison to GRB observations, either this is required or a drastic change in the currently-predicted star history at high redshift (or both) is necessary. Many of the progenitor scenarios for long-duration gamma-ray bursts require binary interactions (for reviews, see Fryer et al 1999Fryer et al , 2007Fryer et al , 2019. If less fragmentation occurs at low metallicities, one might expect fewer binaries and, hence, fewer GRBs (Belczynski et al 2010).…”

Section: Metallicity Effects On Star Formationmentioning

confidence: 99%

Properties of High-Redshift GRBs

Fryer,

Lien,

Fruchter

et al. 2021

Preprint

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The immense power of gamma-ray bursts (GRBs) make them ideal probes of the early universe. By using absorption lines in the afterglows of high-redshift GRBs, astronomers can study the evolution of metals in the early universe. With an understanding of the nature of GRB progenitors, the rate and properties of GRBs observed at high redshift can probe the star formation history and the initial mass function of stars at high redshift. This paper presents a detailed study of the metallicity-and massdependence of the properties of long-duration GRBs under the black-hole accretion disk paradigm to predict the evolution of these properties with redshift. These models are calibrated on the current GRB observations and then used to make predictions for new observations and new missions (e.g. the proposed Gamow mission) studying high-redshift GRBs.

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Understanding the engines and progenitors of gamma-ray bursts

Cited by 31 publications

References 109 publications

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Constraining properties of neutron star merger outflows with radio observations

Properties of High-Redshift GRBs

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