39 research outputs found
Fast spectral variability of GRBs with known redshifts
The fast spectral variability of gamma-ray bursts (GRBs) with known redshifts is investigated using the Konus-Wind experiment data in time scale up to 2ms. Tracks of these GRBs in the luminosity-peak energy plane (Liso,EP ) in the rest-frame are obtained. The distribution of maximum values of an instantaneous luminosity in the GRB’s rest frame Liso is derived for such GRBs depending on the peak energy EP
Observations of giant outbursts from Cygnus X-1
We present interplanetary network localization, spectral, and time history
information for 7 episodes of exceptionally intense gamma-ray emission from
Cygnus X-1. The outbursts occurred between 1995 and 2003, with durations up to
\~28000 seconds. The observed 15 - 300 keV peak fluxes and fluences reached
3E-7 erg /cm2 s, and 8E-4 erg / cm2 respectively. By combining the
triangulations of these outbursts we derive an ~1700 square arcminute (3 sigma)
error ellipse which contains Cygnus X-1 and no other known high energy sources.
The outbursts reported here occurred both when Cyg X-1 was in the hard state as
well as in the soft one, and at various orbital phases. The spectral data
indicate that these outbursts display the same parameters as those of the
underlying hard and soft states, suggesting that they represent another
manifestation of these states.Comment: 27 pages, 9 figures. Revised version. Accepted for publication in the
Astrophysical Journal, tentatively scheduled for October 20, 2003 Part
Multi-Wavelength Studies of the Optically Dark Gamma-Ray Burst 001025A
We identify the fading X-ray afterglow of GRB 001025A from XMM-Newton
observations obtained 1.9-2.3 days, 2 years, and 2.5 years after the burst. The
non-detection of an optical counterpart to an upper limit of R=25.5, 1.20 days
after the burst, makes GRB 001025A a ``dark'' burst. Based on the X-ray
afterglow spectral properties of GRB 001025A, we argue that some bursts appear
optically dark because their afterglow is faint and their cooling frequency is
close to the X-ray band. This interpretation is applicable to several of the
few other dark bursts where the X-ray spectral index has been measured. The
X-ray afterglow flux of GRB 001025A is an order of magnitude lower than for
typical long-duration gamma-ray bursts. The spectrum of the X-ray afterglow can
be fitted with an absorbed synchrotron emission model, an absorbed thermal
plasma model, or a combination thereof. For the latter, an extrapolation to
optical wavelengths can be reconciled with the R-band upper limit on the
afterglow, without invoking any optical circumburst absorption, provided the
cooling frequency is close to the X-ray band. Alternatively, if the X-ray
afterglow is due to synchrotron emission only, seven magnitudes of extinction
in the observed R-band is required to meet the R-band upper limit, making GRB
001025A much more obscured than bursts with detected optical afterglows. Based
on the column density of X-ray absorbing circumburst matter, an SMC gas-to-dust
ratio is insufficient to produce this amount of extinction. The X-ray tail of
the prompt emission enters a steep temporal decay excluding that the tail of
the prompt emission is the onset of the afterglow (abridged).Comment: 32 pages, 8 figures, ApJ in pres
On the Possibility of Identification of a Short/Hard Burst GRB 051103 with the Giant Flare from a Soft Gamma Repeater in the M81 Group of Galaxies
The light curve, energy characteristics, and localization of a short/hard GRB
051103 burst are considered. Evidence in favor of identifying this event with a
giant flare from a soft gamma repeater in the nearby M81 group of interacting
galaxies is discussed.Comment: 11 pages, 4 figures, accepted for publication in Astronomy Letters,
correction of a typo on page
Giant Flare in SGR 1806-20 and Its Compton Reflection from the Moon
We analyze the data obtained when the Konus-Wind gamma-ray spectrometer
detected a giant flare in SGR 1806-20 on December 27, 2004. The flare is
similar in appearance to the two known flares in SGR 0526-66 and SGR 1900+14
while exceeding them significantly in intensity. The enormous X-ray and
gamma-ray flux in the narrow initial pulse of the flare leads to almost
instantaneous deep saturation of the gamma-ray detectors, ruling out the
possibility of directly measuring the intensity, time profile, and energy
spectrum of the initial pulse. In this situation, the detection of an
attenuated signal of Compton back-scattering of the initial pulse emission by
the Moon with the Helicon gamma-ray spectrometer onboard the Coronas-F
satellite was an extremely favorable circumstance. Analysis of this signal has
yielded the most reliable temporal, energy, and spectral characteristics of the
pulse. The temporal and spectral characteristics of the pulsating flare tail
have been determined from Konus-Wind data. Its soft spectra have been found to
contain also a hard power-law component extending to 10 MeV. A weak afterglow
of SGR 1806-20 decaying over several hours is traceable up to 1 MeV. We also
consider the overall picture of activity of SGR 1806-20 in the emission of
recurrent bursts before and after the giant flare.Comment: 29 pages including 18 figures; to appear in Astronomy Letters, 2007,
33, p 1-1