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

Method for Osteosynthesis of Long Tubular Bones Using a Distraction-Reposition Apparatus of External Fixation

Over the past decades, the problem of treating multiple fractures of the limb bones has been the focus of attention of most orthopedic traumatologists in our country and abroad. The urgency of the problem is also determined by the fact that the nature of injuries and their consequences changes with a tendency to increase. Qualitative changes in the structure of injuries are due to an increase in the level of multiple and associated injuries. The use of sequential osteosynthesis in patients with fractures of the long tubular bones of the extremities implies primary stabilization of bone fragments with an externalfixation device and repeated immersion osteosynthesis, when it is possible to achieve stabilization of the patient's condition. There are various rod and pin devices for fixation, some of them are for fixing (which are necessary to remove before the operation), some for preliminary reposition of the fracture during the operation (necessary to remove the skeletal traction or plaster cast and apply the apparatus, which only adds steps to the procedure). The proposed technique is notable for its simple assembly and application, as well as its ease of construction, which ensures patient mobility and allows the patient to stabilize without imperfections and perform final immersion osteosynthesis

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