Origins of Short Gamma-Ray Bursts Deduced from Offsets to Their Host Galaxies Revisited

Cui, Xiaohong; Aoi, Junichi; Nagataki, Shigehiro; Xu, Renxin

doi:10.1063/1.3509250

Cited by 5 publications

(4 citation statements)

References 1 publication

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“…The best fit for ¼ 2:3 is obtained for 90% protons and 10% iron, and %4 G magnetic field coherent on 0.2 kpc scale. For the case of short GRBs (iii), the distribution of sources can be obtained from observations [19]. The spectra obtained in this case are similar to those shown in Fig.…”

supporting

confidence: 67%

Role of Galactic Sources and Magnetic Fields in Forming the Observed Energy-Dependent Composition of Ultrahigh-Energy Cosmic Rays

2010

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Recent results from the Pierre Auger Observatory, showing energy-dependent chemical composition of ultrahigh-energy cosmic rays (UHECRs) with a growing fraction of heavy elements at high energies, suggest a possible non-negligible contribution of the Galactic sources. We show that, in the case of UHECRs produced by gamma-ray bursts or rare types of supernova explosions that took place in the Milky Way in the past, the change in UHECR composition can result from the difference in diffusion times for different species. The anisotropy in the direction of the Galactic center is expected to be a few per cent on average, but the locations of the most recent or closest bursts can be associated with observed clusters of UHECRs.

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supporting

confidence: 67%

Role of Galactic Sources and Magnetic Fields in Forming the Observed Energy-Dependent Composition of Ultrahigh-Energy Cosmic Rays

2010

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“…This is consistent with previous works (e.g. Zhang et al, 2009a;Virgili et al, 2011;Cui et al, 2012) that arrived at this conclusion using very different arguments. The host galaxy data, on the other hand, suggest that contamination of massive star GRBs in the short GRB sample may not be large (Fong et al, 2010;Berger, 2014).…”

Section: Two Physically Distinct Types Of Grbssupporting

confidence: 93%

“…Later, an observer-frame short GRB 090426 at z = 2.609 was discovered, which shared many properties of long GRBs with a massive star origin (Levesque et al, 2010;Antonelli et al, 2009;Xin et al, 2011;Thöne et al, 2011). Independent arguments suggest that at least some short GRBs, especially those at high redshifts with high luminosities, are probably not related to compact star mergers (Zhang et al, 2009a;Virgili et al, 2011;Cui et al, 2012;Bromberg et al, 2012). Bromberg et al (2012) found that there exists a plateau in the dN/dT 90 duration distribution of GRBs (for all samples with different detectors) and argued that this is an evidence for a massive star origin; the plateau, according to them, is due to the finite time it takes for GRB jets to clear a cavity and make their way out of the star.…”

Section: Two Physically Distinct Types Of Grbsmentioning

confidence: 99%

The Physics of Gamma-Ray Bursts and Relativistic Jets

Kumar,

Zhang

2014

Preprint

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We provide a comprehensive review of major developments in our understanding of gamma-ray bursts, with particular focus on the discoveries made within the last fifteen years when their true nature was uncovered. We describe the observational properties of photons from the radio to multi-GeV bands, both in the prompt emission and the afterglow phases. Mechanisms for the generation of these photons in GRBs are discussed and confronted with observations to shed light on the physical properties of these explosions, their progenitor stars and the surrounding medium. After presenting observational evidence that a powerful, collimated, jet moving at close to the speed of light is produced in these explosions, we describe our current understanding regarding the generation, acceleration, and dissipation of the jet. We discuss mounting observational evidence that long duration GRBs are produced when massive stars die, and that at least some short duration bursts are associated with old, roughly solar mass, compact stars. The question of whether a black-hole or a strongly magnetized, rapidly rotating neutron star is produced in these explosions is also discussed. We provide a brief summary of what we have learned about relativistic collisionless shocks and particle acceleration from GRB afterglow studies, and discuss the current understanding of radiation mechanism during the prompt emission phase. We discuss theoretical predictions of possible high-energy neutrino emission from GRBs and the current observational constraints. Finally, we discuss how these explosions may be used to study cosmology, e.g. star formation, metal enrichment, reionization history, as well as the formation of first stars and galaxies in the universe.

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“…For a millisecond pulsar formed by a binary merger, we can take the mass of the neutron star to be M NS = 2.1 M ⊙ (Nice et al 2005) and estimate I 45 ∼ 1.5. Although GRB 090515 has many properties similar to other SGRBs suggesting the progenitor is most likely a compact binary merger, there have been predictions that collapsars may also produce an SGRB (for example, from an orphan precursor jet, Janiuk, Moderski & Proga 2008) and evidence that a significant fraction of SGRBs are related to collapsars rather than compact binary mergers (Virgili et al 2009; Cui, Aoi & Nagataki 2010). So in the following analysis we compare both progenitor models.…”

Section: Discussionmentioning

confidence: 99%

The unusual X-ray emission of the short Swift GRB 090515: evidence for the formation of a magnetar?

Rowlinson¹,

O’Brien²,

Tanvir³

et al. 2010

Monthly Notices of the Royal Astronomical Society

225

240

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The majority of short gamma‐ray bursts (SGRBs) are thought to originate from the merger of compact binary systems collapsing directly to form a black hole. However, it has been proposed that both SGRBs and long gamma‐ray bursts (LGRBs) may, on rare occasions, form an unstable millisecond pulsar (magnetar) prior to final collapse. GRB 090515, detected by the Swift satellite was extremely short, with a T90 of 0.036 ± 0.016 s, and had a very low fluence of 2 × 10−8 erg cm−2 and faint optical afterglow. Despite this, the 0.3–10 keV flux in the first 200 s was the highest observed for an SGRB by the Swift X‐ray Telescope (XRT). The X‐ray light curve showed an unusual plateau and steep decay, becoming undetectable after ∼500 s. This behaviour is similar to that observed in some long bursts proposed to have magnetars contributing to their emission. In this paper, we present the Swift observations of GRB 090515 and compare it to other gamma‐ray bursts (GRBs) in the Swift sample. Additionally, we present optical observations from Gemini, which detected an afterglow of magnitude 26.4 ± 0.1 at T+ 1.7 h after the burst. We discuss potential causes of the unusual 0.3–10 keV emission and suggest it might be energy injection from an unstable millisecond pulsar. Using the duration and flux of the plateau of GRB 090515, we place constraints on the millisecond pulsar spin period and magnetic field.

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Origins of Short Gamma-Ray Bursts Deduced from Offsets to Their Host Galaxies Revisited

Cited by 5 publications

References 1 publication

Role of Galactic Sources and Magnetic Fields in Forming the Observed Energy-Dependent Composition of Ultrahigh-Energy Cosmic Rays

Role of Galactic Sources and Magnetic Fields in Forming the Observed Energy-Dependent Composition of Ultrahigh-Energy Cosmic Rays

The Physics of Gamma-Ray Bursts and Relativistic Jets

The unusual X-ray emission of the short Swift GRB 090515: evidence for the formation of a magnetar?

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