3 keV to 2 MeV observations of four gamma-ray bursts

Laros, J. G.; Evans, W. D.; Fenimore, E.; Klebesadel, R. W.; Shulman, Seth; Fritz, G.

doi:10.1086/162643

Cited by 44 publications

(21 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…MacFadyen & Woosley (1999), MacFadyen et al (2001) and Zhang, Woosley & MacFadyen (2003) have suggested that shock breakout might lead to the X‐ray precursors seen in some bursts (Laros et al 1984; Murakami et al 1991; in 't Zand et al 1999). MacFadyen & Woosley and MacFadyen et al concentrate on the prompt flash from the shock‐heated stellar photosphere; however, the fast ejecta have a greater store of kinetic energy to be tapped.…”

Section: Breakout and Blowout: Observational Consequencesmentioning

confidence: 99%

Supernova hosts for gamma-ray burst jets: dynamical constraints

Matzner

2003

Monthly Notices RAS

226

252

View full text Add to dashboard Cite

I constrain a possible supernova origin for gamma‐ray bursts (GRBs) by modelling the dynamical interaction between a relativistic jet and a stellar envelope surrounding it. The delay in observer time introduced by the jet traversing the envelope should not be long compared with the duration of gamma‐ray emission; also, the jet should not be swallowed by the spherical explosion it powers. The only stellar progenitors that comfortably satisfy these constraints, if one assumes that jets move ballistically within their host stars, are compact carbon–oxygen or helium post‐Wolf–Rayet stars (type Ic or Ib supernovae); type II supernovae are ruled out. Notably, very massive stars do not appear to be capable of producing the observed bursts at any redshift unless the stellar envelope is stripped prior to collapse. The presence of a dense stellar wind places an upper limit on the Lorentz factor of the jet in the internal shock model; however, this constraint may be evaded if the wind is swept forward by a photon precursor. Shock breakout and cocoon blowout are considered individually; neither presents a likely source of precursors for cosmological GRBs. These envelope constraints could conceivably be circumvented if jets are laterally pressure‐confined while traversing the outer stellar envelope. If so, jets responsible for observed GRBs must have been launched from a region several hundred kilometres wide, have been crossed by strong shocks, or have mixed with envelope material as they travel. A phase of pressure confinement and mixing would imprint correlations among jets that may explain observed GRB variability–luminosity and lag–luminosity correlations.

show abstract

Section: Breakout and Blowout: Observational Consequencesmentioning

confidence: 99%

Supernova hosts for gamma-ray burst jets: dynamical constraints

Matzner

2003

Monthly Notices RAS

226

252

View full text Add to dashboard Cite

show abstract

“…The original definitions were ostensibly ''-rays seen before the pulse that triggered the instrument'' or ''X-rays seen before the -rays.'' The term ''precursor'' has been applied to -ray pulses before the event that triggered BATSE ( Koshut et al 1995) and to the slow onset of soft X-ray emission before the main -ray pulse (e.g., GRB 900623; Murakami et al 1991), as well as to isolated X-ray pulses before the GRB itself (e.g., GRB 790307; Laros et al 1984). Koshut et al (1995) defined a precursor to be emission that precedes the main burst by at least the duration of the main burst; using this restrictive definition and BATSE DISCLA data with E > 25 keV, they found that the distribution of ''precursor'' spectral parameters is not significantly different from the distribution of GRB spectral parameters.…”

Section: Precursorsmentioning

confidence: 99%

HETEObservations of the Gamma‐Ray Burst GRB 030329: Evidence for an Underlying Soft X‐Ray Component

Vanderspek

Sakamoto

Barraud

et al. 2004

ApJ

Self Cite

View full text Add to dashboard Cite

An exceptionally intense gamma-ray burst, GRB 030329, was detected and localized by the instruments on board the High Energy Transient Explorer satellite (HETE ) at 11:37:14 UT on 2003 March 29. The burst consisted of two $10 s pulses of roughly equal brightness and an X-ray tail lasting more than 100 s. The energy fluence in the 30-400 keV energy band was S ¼ 1:2 ; 10 À4 ergs cm À2 , making GRB 030329 one of the brightest GRBs ever detected. Communication of a 2 0 error box 73 minutes after the burst allowed the rapid detection of a counterpart in the optical, X-ray, and radio and the ensuing discovery of a supernova with most unusual characteristics. Analyses of the burst light curves reveal the presence of a distinct, bright, soft X-ray component underlying the main GRB; the 2-10 keV fluence of this component is $7 ; 10 À6 ergs cm À2 . The main pulses of GRB 030329 were preceded by two soft, faint, nonthermal bumps. We present details of the HETE observations of GRB 030329.

show abstract

“…A promising experiment on the P78-1 satellite monitored ~ 20 ~o of the sky with every 6 s rotation of the spacecraft; almost the whole sky was covered in an annual cycle, with exposures of 1-2 months on typical sources. Unfortunately, the 6 yr of data are still not analyzed, except for a few observations of X-ray counterparts to gamma bursts (Laros, 1984).…”

Section: Instrumentationmentioning

confidence: 99%

Long-term cycles in cosmic X-ray sources

Priedhorsky

Holt

1987

Space Sci Rev

View full text Add to dashboard Cite

Most of what we know about galactic X-ray binaries comes from their time variation, particularly periodic variations corresponding to neutron star rotation, and binary motion. Longer cycles or quasi-cycles are much harder to observe because of the shortage of instrumentation suitable for long-term monitoring. Nonetheless, cycle with periods up to a few years have been seen in several galactic binaries.Cycles of ~ 30-300 days have been confirmed for four high-mass systems, LMC X-4, Her X-l, SS433, and Cyg X-l, and are suspected in several others. These cycles are observed in both the X-ray and optical bands, and represent cyclic variations in both the inner and outer parts of the accretion disk. Some component of these systems is precessing, but we are not certain which. It could be a misaligned companion star; the outer rim of the accretion disk, driven by radiative feedback; or the neutron star.Several low-mass X-ray binaries have quasi-periodic cycles, with periods ranging from 89 to 2 years. The amplitude of modulation ranges between ~ 50 and 100 ~o, i.e., both 'persistent' and 'transient' objects fall into this class. This activity is reminiscent of the superoutburst cycles of the SU UMa cataclysmic variables, and may be caused by similar mass-transfer instabilities.Periodic outbursts in the Be/neutron star systems seem to result from variable mass transfer in a wide, eccentric orbit. The relationship between the orbital cycle and the flux outbursts, however, is not well understood, and even the equivalence of the outburst and binary cycles remains hypothetical for most objects. Most likely, the periodic outbursts result from enhanced mass transfer at periastron.Compared to other aspects of X-ray astronomy, long-term activity has been much less intensively studied by both observers and theoreticians. A simple all-sky monitor in permanent operation could provide for the X-ray sky the same kind of data base provided to optical observers by the Harvard plates.

show abstract

3 keV to 2 MeV observations of four gamma-ray bursts

Cited by 44 publications

References 0 publications

Supernova hosts for gamma-ray burst jets: dynamical constraints

Supernova hosts for gamma-ray burst jets: dynamical constraints

HETEObservations of the Gamma‐Ray Burst GRB 030329: Evidence for an Underlying Soft X‐Ray Component

Long-term cycles in cosmic X-ray sources

Contact Info

Product

Resources

About