The afterglow, redshift and extreme energetics of the γ-ray burst of 23 January 1999

Kulkarni, [No Value]; Djorgovski, S. G.; Odewahn, SC; Bloom, J.; Gal, R. R.; Koresko, C.; Harrison, F.; Lubin, L. M.; Armus, L.; Sari, Re’em; Illingworth, G. D.; Kelson, D. D.; Magee, D.; Dokkum, PG van; Frail, D. A.; Mulchaey, J.; Malkan, M. A.; McClean, IS; Teplitz, H. I.; Koerner, D. W.; Kirkpatrick, Davy; Kobayashi, Naoto; Yadigaroglu, I. A.; Halpern, J. P.; Piran, Tsvi; Goodrich, R. W.; Chaffee, F. H.; Feroci, M.; Costa, E.

doi:10.1038/18821

Cited by 400 publications

(293 citation statements)

References 44 publications

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“…However, in a number of well monitored cases a change in the light decay rate at about 0.5-1 days after the GRB was detected with a transition to a steeper power law behaviour. The power law indices before and after the temporal break are typically in the range 0.7-1 and 1.7-2.4, respectively (GRB990123: Fruchter et al 1999;Castro-Tirado et al 1999;Kulkarni et al 1999;GRB990510: Stanek et al 1999;Harrison et al 1999;Israel et al 1999;GRB990705: Masetti et al 2000a;GRB000926: Fynbo et al 2001a). This behaviour can be caused by the deceleration of a relativistic jet in a homogeneous medium (Sari et al 1999;Rhoads 1999), or by expansion in a wind (Chevalier & Li 1999, or by the transition between relativistic and Newtonian conditions in the plasma expansion (Dai & Lu 1999).…”

Section: Introductionmentioning

confidence: 99%

GRB010222: Afterglow emission from a rapidly decelerating shock

Masetti¹,

Palazzi²,

Pian³

et al. 2001

A&A

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Abstract. The GRB010222 optical and near-infrared (NIR) afterglow was monitored at the TNG and other Italian telescopes starting ∼1 day after the high-energy prompt event. The BV R light curves, which are the best sampled, are continuously steepening and can be described by two power laws, f (t) ∝ t −α , of indices α1 ∼ 0.7 and α2 ∼ 1.3 before and after a break occurring at about 0.5 days after the GRB start time, respectively. This model accounts well also for the flux in the U , I and J bands, which are less well monitored. The temporal break appears to be achromatic. The two K-band points are not consistent with the above behaviour, and rather suggest a constant trend. A low-resolution optical spectrum has also been taken with TNG. In the optical spectrum we found three absorption systems at different redshifts (0.927, 1.155 and 1.475), the highest of which represents a lower limit to, and probably coincides with, the redshift of the GRB. The broad-band optical spectral energy distributions do not appear to vary with time, consistently with the achromatic behaviour of the light curves. We compare our measurements with different afterglow evolution scenarios and we find that they favor a transition from relativistic to non-relativistic conditions in the shock propagation.

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Section: Introductionmentioning

confidence: 99%

GRB010222: Afterglow emission from a rapidly decelerating shock

Masetti¹,

Palazzi²,

Pian³

et al. 2001

A&A

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“…It has been argued that the rapid temporal decay of several GRB afterglows is more consistent with the evolution of a relativistic jet after it slows down and spreads laterally than with a spherical blast wave [9]. The lack of a significant radio afterglow in GRB 990123 provides independent evidence for jet-like geometry [10].…”

Section: Motivation and Numerical Setupmentioning

confidence: 63%

Relativistic Jets from Collapsars

Aloy¹,

Müeller²,

Ibanyez³

et al. 2001

Godunov Methods

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We have studied the relativistic beamed outflow proposed to occur in the collapsar model of gamma-ray bursts. A jet forms as a consequence of an assumed energy deposition of ∼ 10 50 − 10 51 erg/s within a 30 • cone around the rotation axis of the progenitor star. The generated jet flow is strongly beamed ( < ∼ few degrees) and reaches the surface of the stellar progenitor (r ≈ 3 10 10 cm) intact. At break-out the maximum Lorentz factor of the jet flow is about 33. Simulations have been performed with the GENESIS multi-dimensional relativistic hydrodynamic code. Motivation and numerical setupVarious catastrophic collapse events have been proposed to explain the energies released in a gamma-ray burst (GRB) including compact binary system mergers [6,13], collapsars [18] and hypernovae [14]. These models all rely on a common engine, namely a stellar mass black hole (BH) which accretes several solar masses of matter from a disk (formed during a merger or by a non-spherical collapse). A fraction of the gravitational binding energy released by accretion is converted into a pair fireball. Provided the baryon load of the fireball is not too large, the baryons are accelerated together with the e + e − pairs to ultra-relativistic speeds (Lorentz factors > 10 2 ; [3]). The existence of such relativistic flows is supported by radio observations of GRB 980425 [8].The dynamics of spherically symmetric relativistic fireballs has been studied by several authors by means of 1D Lagrangian hydrodynamic simulations (e.g., [12]). It has been argued that the rapid temporal decay of several GRB afterglows is more consistent with the evolution of a relativistic jet after it slows down and spreads laterally than with a spherical blast wave [9]. The lack of a significant radio afterglow in GRB 990123 provides independent evidence for jet-like geometry [10]. Motivated by these observations and by the collapsar model of [11], we have simulated the propagation of jets from collapsars using relativistic hydrodynamics.In [11] the continued evolution of rotating helium stars, whose iron core collapse does not produce a successful outgoing shock but instead forms a BH surrounded 1

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“…Evidence of a break from a shallow to a steep power law was seen in GRB 990123 [4,20], unfortunately the break was observed only in one optical band while data on other bands were ambiguous. A very clear break was seen in GRB 990510 [21,22] simultaneously in all optical bands and in radio.…”

Section: Jets and Beamingmentioning

confidence: 99%

“…Additionally, Rhoads [19] has shown that at about the same time, the physical size of the jet will begin to increase so that 9(t) ~ 1/7. Taking this effect into account, the break is even more significant and the decay is proportional to t~p ~ t~2 >2 -t~2* 4 .…”

Section: Jets and Beamingmentioning

confidence: 99%

Gamma-ray Bursts and Afterglow

Sari

2000

Symp. - Int. Astron. Union

Self Cite

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Abstract. The origin of GRBs have been a mystery for almost 30 years. Their sources emit a huge amount of energy on short time scales and the process involves extreme relativistic motion with bulk Lorentz factor of at least a few hundred. In the last two years, "afterglow", emission in X-ray, optical, IR, and radio was detected. The afterglow can be measured up to months and even years after the few seconds GRB. We review the theory for the 7-rays emission and the afterglow and show that it is strongly supported by observations. A recent detection of optical emission simultaneous with the GRB, well agrees with theoretical predictions and further constrains the free parameters of the models. We discuss the evidence that some of the bursts are jets, and discuss the prospects of polarization measurements.

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The afterglow, redshift and extreme energetics of the γ-ray burst of 23 January 1999

Cited by 400 publications

References 44 publications

GRB010222: Afterglow emission from a rapidly decelerating shock

GRB010222: Afterglow emission from a rapidly decelerating shock

Relativistic Jets from Collapsars

Gamma-ray Bursts and Afterglow

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