147 research outputs found
Log N-log S in inconclusive
The log N-log S data acquired by the Pioneer Venus Orbiter Gamma Burst Detector (PVO) are presented and compared to similar data from the Soviet KONUS experiment. Although the PVO data are consistent with and suggestive of a -3/2 power law distribution, the results are not adequate at this state of observations to differentiate between a -3/2 and a -1 power law slope
Match Probability Statistics and Gamma Ray Burst Recurrences in the BATSE Catalog
We develop match probability statistics to test the recurrences of gamma ray
bursts in the BATSE catalog 1B and 2B. We do not find a signal of repetitions
at the match level of 1.e-3.Comment: 4 pages, LaTeX, two macros included (kluwer.sty, spacekap.sty) To
appear in the proceedings of the Eslab29 symposium, ``gamma ray bursts:
toward the source
X-ray and low energy gamma-ray observations of the 16 February 1984 solar flare
The February 16, 1984 (0900 UT) solar flare was very energetic and produced a variety of emissions. The X-ray and gamma ray continuum measurement, made aboard the International Cometary Explorer (ICE) and the Pioneer Venus Orbiter (PVO), are briefly described
Soft-spectrum gamma-ray bursts
A typical gamma to ray burst (GRB), when observed over the approximately 30 keV to 1 MeV range, has a 1 to 10 s duration and a spectrum describable in terms of a several-hundred-keV exponential function. However, KONUS data indicate that some GRBs may belong to a separate class of short (approximately 0.1 s), soft (kT 50 keV) events. This result has been questioned because the KONUS experiments, with only 4 s spectral time resolution and a lack of information approximately 30 keV, are not particularly well suited for the detection and study of these bursts. The UC Berkely/Los Alamos Solar X-Ray Spectrometer/GRB experiment on the International Cometry Explorer (ICE), with nearly continuous coverage of approxiomately one-sixth of the sky down to 5 keV at 0.5 s resolution, is better designed for such a task. Using ICE data, it was confirmed that soft-spectrum events do indeed exist, apparently with properties that set them apart from the general GRB population. Results from the ICE experiment are presented
Study of the Correlations Between the Highest Energy Cosmic Ray Showers and Gamma Ray Bursts
We examine the correlation between the arrival direction of ultra high energy
cosmic ray showers and gamma ray bursts in the third BATSE catalog. We find no
correlation between the two data sets. We also find no correlations between a
pre-BATSE burst catalog and the Haverah Park Ultra High Energy shower set that
cover approximately the same period of time.Comment: 1 uuencoded g-zipped postscript file containing text and figure
Relativistic magnetospheric electrons: Lower ionospheric conductivity and long-term atmospheric variability
Long term observations of relativistic electrons in the earth's outer magnetosphere show a strong solar cycle dependence with a prominent intensity maximum during the approach to solar minimum. This population therefore closely corresponds to the presence of high speed solar wind streams emanating from solar coronal holes. Using a numerical code, the precipitating electron energy deposition in the earth's upper and middle atmosphere were calculated. Observed events (typically persisting several days) would have maximum effect in the 40 to 60 km altitude range with peak energy depositions greater than 110 keV/cu cm-s. It is suggested that this electron population could play an important long term role in modulating lower D region ionization and middle atmospheric ozone chemistry. Methods are described of observing middle atmospheric and lower ionospheric effects of the electrons including balloon, riometer, and space-based ozone sensor systems. A particularly promising approach may involve the monitoring of global Schumann resonance modes which are sensitive to global changes in the properties of the earth-ionosphere cavity. Present work indicates that Schumann resonance properties are moderately correlated with the flux of precipitating relativistic electrons thus offering the possibility of continuously monitoring this aspect of magnetosphere-atmosphere coupling
Helios-2 Vela-Ariel-5 gamma-ray burst source position
The gamma-ray burst of 28 January 1976, one of 18 events thus far detected in interplanetary space with Helios-2, was also observed with the Vela-5A, -6A and the Ariel-5 satellites. A small source field is obtained from the intersection of the region derived from the observed time delays between Helios-2 and Vela-5A and -6A with the source region independently found with the Ariel-5 X-ray detector. This area contains neither any steady X-ray source as scanned by HEAO-A nor any previously catalogued X-ray, radio or infrared sources, X-ray transients, quasars, seyferts, globular clusters, flare stars, pulsars, white dwarfs or high energy gamma-ray sources. The region is however, within the source field of a gamma-ray transient observed in 1974, which exhibited nuclear gamma-ray line structure
The 1979, March 5 Gamma-Ray Transient: Was it a Classic Gamma-Ray Burst?
The March 5th, 1979 gamma-ray transient has long been thought to be
fundamentally different from the classic gamma-ray bursts (GRBs). It had
recurrences, pulsations, and a soft spectral component unlike classic GRBs.
With the exception of the soft component reported from the Konus experiment,
the unusual characteristics of March 5th were detectable main peak differs
markedly from the published Konus spectrum. Rather than being dominated by a
soft component similar to that observed in the soft gamma repeaters (SGRs), the
ICE-PVO spectrum appears to be consistent with a classic GRB spectrum,
especially above 100 keV. We believe that, given the ICE-PVO spectral
observations, the March 5th transient would have been classified as a classic
GRB when it was discovered.
The SGRs and GRBs could be consanguineous: high-velocity neutron stars
initially produce SGR events (and, occasionally a GRB like March 5th) and when
they are older and in the galactic corona, they go through a GRB phase. The
March 5th event demonstrates that high-velocity neutron stars at distances of
tens kpc are capable of producing events like classic GRBs.Comment: 32 pages, uuencoded Postscript with figures. Also available via ftp
at ftp://nis-ftp.lanl.gov/pub/grb/march5.p
Stellar explosions powered by the Blandford-Znajek mechanism
In this letter we briefly describe the first results of our numerical study
on the possibility of magnetic origin of relativistic jets of long duration
gamma ray bursters within the collapsar scenario. We track the collapse of
massive rotating stars onto a rotating central black hole using axisymmetric
general relativistic magnetohydrodynamic code that utilizes a realistic
equation of state of stellar matter, takes into account the cooling associated
with emission of neutrinos, and the energy losses due to dissociation of
nuclei. The neutrino heating is not included. We describe the solution for one
particular model where the progenitor star has magnetic field G. The
solution exhibits strong explosion driven by the Poynting-dominated jets whose
power exceeds . The jets originate mainly from the
black hole and they are powered via the Blandford-Znajek mechanism. The full
details of the simulations together with the results of parameter study will be
presented elsewhere. A number of simulation movies can be downloaded from
http://www.maths.leeds.ac.uk/~serguei/research/movies/anim.htmlComment: minor revision, accepted by MNRAS Letters, simulation movies can be
downloaded from
http://www.maths.leeds.ac.uk/~serguei/research/movies/anim.htm
The cepheid-like relationship between variability and luminosity explained within the ``cannonball model'' of Gamma-Ray bursts
I show how an empirical variability - luminosity relationship for prompt
gamma-ray bursts, first proposed by Fenimore and Ramirez-Ruiz, can be
understood as a special-relativistic beaming effect in the ``cannonball model''
of Dar and De R\'ujula. In this scenario the variability is a measure of the
direction of propagation and the Lorentz factor of the cannonball on which in
turn the apparent luminosity of the prompt GRB depends sensitively. The
observed absence of cosmological time dilation in the ``aligned peak test'' -
when using redshifts derived with this relation - is also explained. The most
direct evidence in favour of the cannonball model presented here is its correct
description for the observed relation between narrow-spike width and amplitude
within a given GRB. There seems to be an indication for cosmological time
dilation in the total duration of GRBs, as expected in the cannonball model.
Quantitative predictions for the luminosity function of GRBs and the
``spectral-lag luminosity relation'' are given.Comment: 7 pages, Latex, 2 eps figures, submitted to Astronomy & Astrophysics,
improved clarity of exposition in section 1.2 and 2.5 of revised versio
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