On the difference between the short and long gamma-ray bursts

Balázs, L. G.; Bagoly, Z.; Horváth, I.; Mészáros, A.; Mészáros, P.

doi:10.1051/0004-6361:20021863

Cited by 70 publications

(93 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…These are reasonable and not extreme values in view of model calculations for the energy release by neutrino-antineutrinoannihilation in case of post-merging BH accretion Janka et al 1999;Setiawan et al 2004). Provided a major fraction of the energy of the ultrarelativistic fireball gets converted to gamma-rays, our maximum isotropic equivalent energies are in good agreement with estimates based on a comparison of the energetics of short and long GRBs, suggesting an approximate fluence-duration proportionality (Balázs et al 2003). Since long bursts last typically about 50−100 times longer, a similar luminosity (e.g., Mao et al 1994; L short iso ∼ L long iso ∼ 10 51−52 erg s −1 ) implies an apparent energy which is around 10 51 erg for short bursts instead of ∼10 53 erg for long ones (Frail et al 1997).…”

Section: Discussionsupporting

confidence: 85%

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Aloy¹,

Janka²,

Müeller³

2005

A&A

253

295

View full text Add to dashboard Cite

Abstract. We present the first general relativistic hydrodynamic models of the launch and evolution of relativistic jets and winds, driven by thermal energy deposition, possibly due to neutrino-antineutrino annihilation, in the close vicinity of black hole-accretion torus systems. The latter are considered to be the remnants of compact object mergers. Our two-dimensional simulations establish the link between models of such mergers and future observations of short gamma-ray bursts by the SWIFT satellite. They show that ultrarelativistic outflow with maximum terminal Lorentz factors around 1000 develops for polar energy deposition rates above some 10 48 erg s −1 per steradian, provided the merger environment has a sufficiently low baryon density. By the interaction with the dense accretion torus the ultrarelativistic outflow with Lorentz factors Γ above 100 is collimated into a sharp-edged cone that is embedded laterally by a wind with steeply declining Lorentz factor. The typical semi-opening angles of the Γ > 100 cone are 5 • −10 • , corresponding to about 0.4−1.5% of the hemisphere and apparent isotropized energies (kinetic plus internal) up to ≈10 51 erg although at most 10−30% of the deposited energy is transferred to the outflow with Γ > 100. The viability of post-merger black hole-torus systems as engines of short, hard gamma-ray bursts is therefore confirmed. The annihilation of neutrino-antineutrino pairs radiated from the hot accretion torus appears as a suitable energy source for powerful axial outflow even if only ≈10 49 erg are deposited within a cone of 45 • half-opening angle around the system axis. Although the torus lifetimes are expected to be only between some 0.01 s and several 0.1 s, our models can explain the durations of all observed short gamma-ray bursts, because different propagation velocities of the front and rear ends will lead to a radial stretching of the ultrarelativistic fireball before transparency is reached. The ultrarelativistic flow reveals a highly non-uniform structure caused by the action of Kelvin-Helmholtz instabilities that originate at the fireball-torus interface. Large radial variations of the baryon density (up to several orders of magnitude) are uncorrelated with moderate variations of the Lorentz factor (factors of a few) and fluctuations of the gently declining radiation-dominated pressure. In the angular direction the Lorentz factor reveals a nearly flat plateau-like maximum with values of several hundreds, that can be located up to 7 • off the symmetry axis, and a steep decrease to less than 10 for polar angles larger than 15 • −20 • . Lateral expansion of the ultrarelativistic core of the flow is prevented by a subsonic velocity component of about 0.05c towards the symmetry axis, whereas the moderately relativistic wings show a subsonic sideways inflation with less than 0.07c (measured in the frame comoving with the radial flow).

show abstract

Section: Discussionsupporting

confidence: 85%

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Aloy¹,

Janka²,

Müeller³

2005

A&A

253

295

View full text Add to dashboard Cite

show abstract

“…Therefore, the redshift-convoluted 4-Dimensional (4D) rest-frame distribution can be well approximated as a linear translation of the observer-frame parameters to the restframe parameter space, keeping the shape of the distribution almost intact (e.g., Balazs et al 2003). This implies that the joint distribution of the intrinsic SGRB variables: the isotropic peak luminosity (Liso), the total isotropic emission (Eiso), the rest-frame time-integrated spectral peak energy (Ep,z) and the rest-frame duration (T90,z) might be indeed well described as a multivariate log-normal distribution.…”

Section: Model Constructionmentioning

confidence: 99%

Short versus long gamma-ray bursts: a comprehensive study of energetics and prompt gamma-ray correlations

Shahmoradi

Nemiroff

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the results of a comprehensive study of the luminosity function, energetics, prompt gamma-ray correlations, and classification methodology of short-hard and long-soft GRBs (SGRBs & LGRBs), based on observational data in the largest catalog of GRBs available to this date: BATSE catalog of 2702 GRBs. We find that: 1. The least-biased classification method of GRBs into short and long, solely based on prompt-emission properties, appears to be the ratio of the observed spectral peak energy to the observed duration (R = E p /T 90 ) with the dividing line at R 50[keV s −1 ]. 2. Once data is carefully corrected for the effects of the detection threshold of gammaray instruments, the population distribution of SGRBs and LGRBs can be individually well described as multivariate log-normal distribution in the 4-dimensional space of the isotropic peak gamma-ray luminosity, total isotropic gamma-ray emission, the intrinsic spectral peak energy, and the intrinsic duration. 3. Relatively large fractions of SGRBs and LGRBs with moderate-to-low spectral peak energies have been missed by BATSE detectors. 4. Relatively strong and highly significant intrinsic hardnessbrightness and duration-brightness correlations likely exist in both populations of SGRBs and LGRBs, once data is corrected for selection effects. The strengths of these correlations are very similar in both populations, implying similar mechanisms at work in both GRB classes, leading to the emergence of these prompt gamma-ray correlations.

show abstract

“…For example, in the BATSE database, three subgroups (short, intermediate, and long GRBs) have been robustly identified (Horváth et al 2006;Chattopadhyay et al 2007, and references therein). The short and long subgroups are physically different phenomena (Balázs et al 2003). However, in contrast to this, it remains possible that the intermediate subgroup is not a true physically independent subgroup and it is present in the BATSE database because of e.g.…”

Section: Introductionmentioning

confidence: 96%

“…We proceed in an identical way to the successful statistical analysis completed for the BATSE catalog (Horváth 1998) leading to the discovery of the third subgroup (Mukherjee et al 1998;Bagoly et al 1998;Horvath 1999;Hakkila et al 2000;Rajaniemi & Mähönen 2002;Horváth 2002Horváth , 2003Balázs et al 2003;Horváth et al 2006;Chattopadhyay et al 2007). A statistical study of the Swift database -using the maximum likelihood method -has already shown evidence of a third subgroup (Horváth et al 2008).…”

Section: Introductionmentioning

confidence: 97%

A comparison of the gamma-ray bursts detected by BATSE and Swift

Huja¹,

Mészáros²,

Řípa³

2009

A&A

Self Cite

View full text Add to dashboard Cite

Aims. The durations of 388 gamma-ray bursts detected by the Swift satellite, are analyzed statistically to search for subgroups. The results are then compared with results obtained earlier for data from the BATSE database. Methods. We apply the standard χ 2 test. Results. As for data in the BATSE database, short and long subgroups are also reliably identified in the Swift data. An intermediate subgroup is also seen in the Swift database.Conclusions. The analysis of the entire sample of 388 GRBs provides a support for the existence of three subgroups.

show abstract

On the difference between the short and long gamma-ray bursts

Cited by 70 publications

References 39 publications

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

Short versus long gamma-ray bursts: a comprehensive study of energetics and prompt gamma-ray correlations

A comparison of the gamma-ray bursts detected by BATSE and Swift

Contact Info

Product

Resources

About