Observations of GRB 990123 by the<i>Compton Gamma Ray Observatory</i>

Briggs, M. S.; Band, D. L.; Kippen, R. M.; Preece, R. D.; Kouveliotou, C.; Paradijs, J. van; Share, G. H.; Murphy, R. J.; Matz, S. M.; Connors, A.; Winkler, Christoph; McConnell, Mark L.; Ryan, J. M.; Williams, O. R.; Young, C. A.; Dingus, B. L.; Catelli, J. R.; Wijers, R. A. M. J.

doi:10.1086/307808

Cited by 114 publications

(80 citation statements)

References 41 publications

(17 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Achromatic temporal breaks in the optical light curves of GRB 990123 (Kulkarni et al 1999) and GRB 990510 (Harrison et al 1999) suggest, however, that the most luminous GRBs might be beamed, so that only directional energy releases are actually measured. In the case of GRB 990123 (Briggs et al 1999), the directional gamma-ray power and gamma-ray energy release reach peak values @L =@ $ 3 Â 10 51 ergs s À1 sr À1 and @E=@ $ 2 Â 10 53 ergs sr À1 , respectively.…”

Section: Introductionmentioning

confidence: 99%

Neutrino, Neutron, and Cosmic‐Ray Production in the External Shock Model of Gamma‐Ray Bursts

Dermer

2002

ApJ

120

113

View full text Add to dashboard Cite

The hypothesis that ultrahigh-energy (e10 19 eV) cosmic rays (UHECRs) are accelerated by gamma-ray burst (GRB) blast waves is assumed to be correct. Implications of this assumption are then derived for the external shock model of GRBs. The evolving synchrotron radiation spectrum in GRB blast waves provides target photons for the photomeson production of neutrinos and neutrons. Decay characteristics and radiative efficiencies of the neutral particles that escape from the blast wave are calculated. The diffuse high-energy GRB neutrino background and the distribution of high-energy GRB neutrino events are calculated for specific parameter sets, and a scaling relation for the photomeson production efficiency in surroundings with different densities is derived. GRBs provide an intense flux of high-energy neutrons, with neutron production efficiencies exceeding $1% of the total energy release. The radiative characteristics of the neutron -decay electrons from the GRB '' neutron bomb '' are solved in a special case. Galaxies with GRB activity should be surrounded by radiation halos of $100 kpc extent from the outflowing neutrons, consisting of a nonthermal optical/X-ray synchrotron component and a high-energy gamma-ray component from Compton-scattered microwave background radiation. The peak luminosity emitted by the diffuse electron halo from a single GRB with e2 Â 10 53 ergs isotropic energy release is $10 35 ergs s À1 , with a potentially much brighter signal from the neutron decay protons. The decay halo from a single GRB can persist for e0.1-1 Myr. Stronger neutrino fluxes and neutron decay halos can be produced by external shocks in clumpy external media and in scenarios involving internal shock scenarios, so detection of neutrinos associated with smooth profile GRBs could rule out an impulsive GRB central engine and an external shock model for the prompt phase. The luminosity of sources of GRBs and relativistic outflows in L* galaxies such as the Milky Way is at the level of $10 40AE1 ergs s À1 . This is sufficient to account for UHECR generation by GRBs. We briefly speculate on the possibility that hadronic cosmic rays originate from the subset of supernovae that collapse to form relativistic outflows and GRBs.

show abstract

Section: Introductionmentioning

confidence: 99%

Neutrino, Neutron, and Cosmic‐Ray Production in the External Shock Model of Gamma‐Ray Bursts

Dermer

2002

ApJ

120

113

View full text Add to dashboard Cite

show abstract

“…To decrease kT ph from 100 keV to 1 eV, a very unrealistic value of λ = (10 −5 ) 4 = 10 −20 is required ! The V band then always lies in the Rayleigh-Jeans part of the photospheric spectrum where dn ph dEdt ∝ E. GRB 990123 has an averaged spectrum which is well reproduced by the Band function with the following parameters : α = −0.6, β = −3.11, Ep = 720 keV and photon flux 1.93 10 −3 ph/s/cm 2 /keV at 1 MeV (Briggs et al 1999). The redshift of the source is z = 1.6.…”

Section: The Optical Photospheric Emissionmentioning

confidence: 91%

The Expected Thermal Precursors of Gamma-Ray Bursts in the Internal Shock Model

Daigne

Mochkovitch

2003

AIP Conference Proceedings

View full text Add to dashboard Cite

The prompt emission of gamma-ray bursts probably comes from a highly relativistic wind which converts part of its kinetic energy into radiation via the formation of shocks within the wind itself. Such "internal shocks" can occur if the wind is generated with a highly non uniform distribution of the Lorentz factor. We estimate the expected photospheric emission of such a relativistic wind when it becomes transparent. We compare this thermal emission (temporal profile + spectrum) to the non-thermal emission produced by the internal shocks. In most cases, we predict a rather bright thermal emission that should already have been detected. This favors acceleration mechanisms for the wind where the initial energy input is under magnetic rather than thermal form. Such scenarios can produce thermal X-ray precursors comparable to those observed by GINGA and WATCH/GRANAT.

show abstract

“…Among these GRBs are GRB 990123 (Akerlof et al 1999;Briggs et al 1999;Sari & Piran 1999a;Soderberg & Ramirez-Ruiz 2002), GRB 050904 (Boër et al 2006), GRB 060124 (Romano et al 2006), GRB 060418 and GRB 060607A (Molinari et al 2007), GRB 061121 ) and also in GRB 041219A (Vestrand et al 2005;Blake et al 2005;McBreen et al 2006). However, for GRB 041219A, GRB 061121 and GRB 041219A, the optical and prompt gamma emission are highly correlated which indicates a common origin.…”

Section: Afterglow and Optical Flashmentioning

confidence: 98%

Fermi/GBM observations of the ultra-long GRB 091024

Gruber

Krühler

Foley

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

Aims. In this paper we examine gamma-ray and optical data of GRB 091024, a gamma-ray burst (GRB) with an extremely long duration of T 90 ≈ 1020 s, as observed with the Fermi Gamma-ray Burst Monitor (GBM). Methods. We present spectral analysis of all three distinct emission episodes using data from Fermi/GBM. Because of the long nature of this event, many ground-based optical telescopes slewed to its location within a few minutes and thus were able to observe the GRB during its active period. We compare the optical and gamma-ray light curves. Furthermore, we estimate a lower limit on the bulk Lorentz factor from the variability and spectrum of the GBM light curve and compare it with that obtained from the peak time of the forward shock of the optical afterglow. Results. From the spectral analysis we note that, despite its unusually long duration, this burst is similar to other long GRBs, i.e. there is spectral evolution (both the peak energy and the spectral index vary with time) and spectral lags are measured. We find that the optical light curve is highly anti-correlated to the prompt gamma-ray emission, with the optical emission reaching the maximum during an epoch of quiescence in the prompt emission. We interpret this behavior as the reverse shock (optical flash), expected in the internal-external shock model of GRB emission but observed only in a handful of GRBs so far. The lower limit on the initial Lorentz factor deduced from the variability time scale (Γ min = 195 +90 −110 ) is consistent within the error to the one obtained using the peak time of the forward shock (Γ 0 = 120) and is also consistent with Lorentz factors of other long GRBs.

show abstract

Observations of GRB 990123 by theCompton Gamma Ray Observatory

Cited by 114 publications

References 41 publications

Neutrino, Neutron, and Cosmic‐Ray Production in the External Shock Model of Gamma‐Ray Bursts

Neutrino, Neutron, and Cosmic‐Ray Production in the External Shock Model of Gamma‐Ray Bursts

The Expected Thermal Precursors of Gamma-Ray Bursts in the Internal Shock Model

Fermi/GBM observations of the ultra-long GRB 091024

Contact Info

Product

Resources

About