Long γ-ray bursts and core-collapse supernovae have different environments

Fruchter, A. S.; Levan, A. J.; Strolger, Louis-Gregory; Vreeswijk, P. M.; Thorsett, S. E.; Bersier, D.; Burud, I.; Cerón, J. M. Castro; Castro-Tirado, A. J.; Conselice, Christopher J.; Dahlén, T.; Ferguson, Henry C.; Fynbo, J. P. U.; Garnavich, P.; Gibbons, R.; Gorosabel, J.; Gull, T. R.; Hjorth, J.; Holland, S. T.; Kouveliotou, C.; Levay, Zoltan G.; Livio, Mario; Metzger, M.; Nugent, P.; Petro, L.; Pian, E.; Rhoads, James E.; Riess, Adam G.; Sahu, K. C.; Smette, A.; Tanvir, N. R.; Wijers, R. A. M. J.; Woosley, S. E.

doi:10.1038/nature04787

Cited by 779 publications

(974 citation statements)

References 52 publications

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“…While the collapsar progenitor in our binary model travels only 200 pc before it dies, compared to the 400...800 pc deduced by Hammer et al (2006), binary evolution resulting in higher runaway velocities are certainly possible (Petrovic et al 2005a). It remains to be analyzed whether the runaway scenario is compatible with the finding that long GRBs are more concentrated in the brightest regions of their host galaxies than core collapse supernovae (Fruchter et al 2006).…”

Section: Effects From Runaway Grbsmentioning

confidence: 77%

Binary star progenitors of long gamma-ray bursts

Cantiello

Yoon

Langer

et al. 2007

A&A

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Context. The collapsar model for long gamma-ray bursts requires a rapidly rotating Wolf-Rayet star as progenitor. Aims. We test the idea of producing rapidly rotating Wolf-Rayet stars in massive close binaries through mass accretion and consecutive quasi-chemically homogeneous evolution -the latter had previously been shown to provide collapsars below a certain metallicity threshold. Methods. We use a 1D hydrodynamic binary evolution code to simulate the evolution of a 16 + 15 M binary model with an initial orbital period of 5 days and SMC metallicity (Z = 0.004). Internal differential rotation, rotationally induced mixing and magnetic fields are included in both components, as well as non-conservative mass and angular momentum transfer, and tidal spin-orbit coupling. Results. The considered binary system undergoes early Case B mass transfer. The mass donor becomes a helium star and dies as a type Ib/c supernova. The mass gainer is spun-up, and internal magnetic fields efficiently transport accreted angular momentum into the stellar core. The orbital widening prevents subsequent tidal synchronization, and the mass gainer rejuvenates and evolves quasichemically homogeneously thereafter. The mass donor explodes 7 Myr before the collapse of the mass gainer. Assuming the binary to be broken-up by the supernova kick, the potential gamma-ray burst progenitor would become a runaway star with a space velocity of 27 km s −1 , traveling about 200 pc during its remaining lifetime. Conclusions. The binary channel presented here does not, as such, provide a new physical model for collapsar production, as the resulting stellar models are almost identical to quasi-chemically homogeneously evolving rapidly rotating single stars. However, it may provide a means for massive stars to obtain the required high rotation rates. Moreover, it suggests that a possibly large fraction of long gamma-ray bursts occurs in runaway stars.

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Section: Effects From Runaway Grbsmentioning

confidence: 77%

Binary star progenitors of long gamma-ray bursts

Cantiello

Yoon

Langer

et al. 2007

A&A

Self Cite

211

250

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“…In particular, the host galaxies of GRBs have a distinct tendency to be subluminous [21] and metal-poor [23]. This has been demonstrated for GRB hosts both locally [24] and at cosmological distances [25], which suggests that low metallicity is a key ingredient in the production of a gamma-ray burst [24]. As we discuss in Section II, a rapidly rotating star, as required in the collapsar model [26], can retain much of its original mass and angular momentum if it is metal-poor [27].…”

Section: Fig 1 (Color Online)mentioning

confidence: 99%

Enhanced cosmological GRB rates and implications for cosmogenic neutrinos

Yüksel

Kistler

2007

Phys. Rev. D

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Gamma-ray bursts, which are among the most violent events in the Universe, are one of the few viable candidates to produce ultra high-energy cosmic rays. Recently, observations have revealed that GRBs generally originate from metal-poor, low-luminosity galaxies and do not directly trace cosmic star formation, as might have been assumed from their association with core-collapse supernovae. Several implications follow from these findings. The redshift distribution of observed GRBs is expected to peak at higher redshift (compared to cosmic star formation), which is supported by the mean redshift of the Swift GRB sample, hzi 3. If GRBs are, in fact, the source of the observed UHECR, then cosmic-ray production would evolve with redshift in a stronger fashion than has been previously suggested. This necessarily leads, through the GZK process, to an enhancement in the flux of cosmogenic neutrinos, providing a near-term approach for testing the gamma-ray burst-cosmic-ray connection with ongoing and proposed UHE neutrino experiments.

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“…Indeed, the few metallicities derived from the nebular line analysis point to sub-solar metallicities (Sollerman et al 2005). The GRB hosts also generally have sub-L * luminosities (Le Floc'h et al 2003;Fruchter et al 2006), consistent with low metallicities. Modjaz et al (2008) has, in addition, shown that GRBs occur in lower metallicity galaxies than the ones hosting a random sample of Type Ic SN.…”

Section: Metallicitymentioning

confidence: 88%

“…At low redshift, the association between the GRBs and massive star progenitors is well established by (i) Type Ic supernovae (SNe) identified at the positions of GRB events (Hjorth et al 2003;Mirabal et al 2006) and (ii) the location of GRBs in Wolf-Rayet galaxies (Hammer et al 2006). At high redshift, the connection between GRBs and star-forming regions is inferred by (i) GRBs found in blue galaxies with nebular lines indicative of on-going star formation (Le Floc'h et al 2003;Prochaska et al 2004) and (ii) GRBs observed within a few kpc from the weighted flux centroid of their host (Fruchter et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Probing the Interstellar Medium and Stellar Environments of Long-Duration GRBs

2007

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Abstract.We review the properties of the gas surrounding high-redshift gamma-ray bursts (GRBs) assessed through the analysis of damped Lyman-alpha systems (DLAs) identified in their afterglow spectra. These GRB-DLAs are characterized by large H I column densities with a median of N (H I) = 10 21. 7 cm −2 , no molecular gas signatures, metallicities ranging from 1/100 to nearly solar with a median exceeding 1/10 solar, and no anomalous abundance patterns. The detection of the atomic Mg lines and the time-variability of the fine-structure lines demonstrates that the majority of the neutral gas along the GRB sightlines is located between 50 pc and a few kpc from the GRB. This implies that this gas is presumably associated with the ambient interstellar medium of the host galaxy and that the derived properties from low-ionization lines do not directly constrain the local environment of the GRB progenitor. The highly ionized gas, traced by N V lines, which could result from a pre-existing H II region produced by the GRB progenitor and neighboring OB stars, appears on the other hand to be very local to the GRB at about 10 pc, yielding a snapshot of the medium's physical conditions at this radius.

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Long γ-ray bursts and core-collapse supernovae have different environments

Cited by 779 publications

References 52 publications

Binary star progenitors of long gamma-ray bursts

Binary star progenitors of long gamma-ray bursts

Enhanced cosmological GRB rates and implications for cosmogenic neutrinos

Probing the Interstellar Medium and Stellar Environments of Long-Duration GRBs

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