Time Profiles Of Bursts Research Articles

Gamma-ray burst engines may have no memory

A sizeable fraction of gamma-ray burst (GRB) time profiles consist of a temporal sequence of pulses. The nature of this stochastic process carries information on how GRB inner engines work. The so-called interpulse time defines the interval between adjacent pulses, excluding the long quiescence periods during which the signal drops to the background level. It was found by many authors in the past that interpulse times are lognormally distributed, at variance with the exponential case that is expected for a memoryless process. We investigated whether the simple hypothesis of a temporally uncorrelated sequence of pulses is really to be rejected, as a lognormal distribution necessarily implies. We selected and analysed a number of multi--peaked CGRO/BATSE GRBs and simulated similar time profiles, with the crucial difference that we assumed exponentially distributed interpulse times, as is expected for a memoryless stationary Poisson process. We then identified peaks in both data sets using a novel peak search algorithm, which is more efficient than others used in the past. We independently confirmed that the observed interpulse time distribution is approximately lognormal. However, we found the same results on the simulated profiles, in spite of the intrinsic exponential distribution. Although intrinsic lognormality cannot be ruled out, this shows that intrinsic interpulse time distribution in real data could still be exponential, while the observed lognormal could be ascribed to the low efficiency of peak search algorithms at short values combined with the limitations of a bin-integrated profile. Our result suggests that GRB engines may emit pulses after the fashion of nuclear radioactive decay, that is, as a memoryless process.

Ionospheric response to the extreme solar burst of October 28, 2003

Using GPS and GLONASS navigation systems, instantaneous observations of solar burst effects on the Earth’s ionosphere are made. These observations are carried out for both Northern and Southern hemispheres, including the ionosphere at polar and equatorial latitudes. It is shown that the rate of total electron content (TEC) change is agrees well with the time profiles of solar bursts. An experimental dependence of the electron content gradient on the elevation angle is obtained.

High-Resolution Time Profiles of Fiber Bursts at 1420 and 2695 MHz

To obtain constraints for models of fiber bursts, high-resolution time (0.01 s) profiles of the fiber bursts recorded at 1420 and 2695 MHz by the Trieste radiometers are studied in detail. The fiber bursts were identified using Ondřejov radio spectra. During the years 2000 – 2005, 18 intervals with fiber bursts were selected; 26 groups were defined and about 700 fibers were analyzed in detail. More than 300 pulsations, present almost simultaneously with the fibers, were also selected and studied in order to find similarities or differences between these two types of fine structures. It was found that the polarization of the associated continuum, both for fiber bursts and pulsations, is practically the same. Evaluating the ratio between absorption over emission of many single fibers we found that this parameter is very different even for nearby bursts; however, we realized that this ratio shows a tendency to decrease with time. Finally, the time profile of one selected fiber burst was fitted using a recent model based on the modulation of the broadband radio emission by fast magnetoacoustic waves. The results are discussed.

RT-2 radio telescope of the Ussuriysk Astrophysical Observatory: current state and observation data

UDC 520.524 An RT-2 radio telescope of the Ussuriysk Astrophysical Observatory (UAO) is intended for measuring the total flux of solar radio emission at a frequency of 2.804 GHz. Regular observations have been carried out in the UAO since 1990. The current state of the instrument and the data survey for the observation years are presented. The emphasis is on the transition to digital registration of the radio flux in 2002, which offers new opportunities of the data analysis. Digital recording allows us to improve the accuracy of the daily radio-flux measurements, ensures their comparison with the data of the integral radio emission at other frequencies, and provides for reconstruction of the time profiles of powerful radio bursts. Possible problems which can be solved using the UAO radiometer data are outlined. Studies of solar activity are very important for understanding of the fundamental aspects of plasma physics and the processes that occur in distant stellar objects. In this case, both long-term observations and studies of sporadic solar events are of interest. They are required to understand and predict the solaractivity influence on the Earth and in the near-Earth space. Solar radio emission is an important source of information on the solar activity. An RT-2 radio telescope of the Ussuriysk Astrophysical Observatory (UAO) is intended for daily measurements of the total flux of solar radio emission at a wavelength of 10.7 cm. The total radiation flux at this wavelength is one of the most important and widely used indices which are utilized for statistical studies of the solar activity. There is a good correlation between the radio-emission flux values at a wavelength of 10.7 cm and the relative number of the sunspots (Wolf numbers), which is the longest series of the solar indices [1, 2]. However, while the series of the everyday Wolf numbers often show abrupt changes in the values due to subjective factors (in particular, related to the appearance of sunspot groups from behind the limb and their disappearance behind the limb) [3]), the total radio-emission flux is registered by the objective methods and the flux variations are smoother. Therefore, this index is more accurate compared with other solar-activity indices. The solar-activity observations were carried out at the Ussuriysk Astrophysical Observatory from 1973 to 1987 at a frequency of 2.930 GHz, whereas regular radio-emission flux measurements at a frequency of 2.804 GHz have started since 1990. Brief description of the measuring instruments is presented in [4] along with the discussion of the first results obtained. Since some changes were introduced into the radiometer recording system, we should provide the users of our data with a more up-to-date information and discuss the recently obtained observation data.

INTEGRAL CONSTRAINTS ON GAMMA-RAY BURST POLARIZATION AND ON THE POPULATION OF NEARBY, LOW-LUMINOSITY BURSTS

The ESA γ-ray astronomy satellite INTEGRAL localized 46 gamma-ray bursts between October 2002 and July 2007. Spectral lags have been determined from the burst time profiles for about half the sample, despite the extreme faintness of many INTEGRAL bursts. INTEGRAL's sensitivity across the energy range of interest for the prompt burst emission allows us to investigate the hypothesis of a low-luminosity, nearby population of bursts. The azimuthal distribution of double-scatter events in SPI's germanium detectors, in conjunction with a sophisticated spacecraft and instrument mass model, have been used to place limits on the percentage of polarization in the prompt emission of the brightest INTEGRAL burst, GRB 041219a.

Searching for very-high-energy gamma-ray bursts from evaporating primordial black holes

Temporal and energy characteristics of the very-high-energy gamma-ray bursts from evaporating primordial black holes have been calculated by assuming that the photospheric and chromospheric effects are negligible. The technique of searching for such bursts on shower arrays is described. We show that the burst time profile and the array dead time should be taken into account to interpret experimental data. Based on data from the Andyrchy array of the Baksan Neutrino Observatory (Institute for Nuclear Research, Russian Academy of Sciences), we have obtained an upper limit on the number density of evaporating primordial black holes in a local region of space with a scale size of ~10^{-3} pc. Comparison with the results of previous experiments is made.

Discovery of X-ray burst triplets in EXO 0748-676

Type-I X-ray bursts are thermonuclear flashes that take place on the surface of accreting neutron stars. The wait time between consecutive bursts is set by the time required to accumulate the fuel needed to trigger a new burst; this is at least one hour. Sometimes secondary bursts are observed, approximately 10 min after the main burst. These short wait-time bursts are not yet understood. We observed the low-mass X-ray binary and X-ray burster EXO 0748-676 with XMM-Newton for 158 h, during 7 uninterrupted observations lasting up to 30 h each. We detect 76 X-ray bursts. Most remarkably, 15 of these bursts occur in burst triplets, with wait times of 12 min between the three components of the triplet, T1, T2, and T3. We also detect 14 doublets with similar wait times between the two components of the doublet, D1 and D2. We characterize this behavior to try and obtain a better understanding of bursts with short wait times. We measure the burst peak flux, fluence, wait time and time profile, and study correlations between these parameters and with the persistent flux representing the mass accretion rate. (i) For all bursts with a long wait time, the fluence is tightly correlated with the wait time, whereas burst with short wait times generally have higher fluences than expected from this relationship; (ii) wait times tend to be longer after doublets and triplets; (iii) the time profile of single bursts, S1, and of the first burst in a double or triple burst, D1 and T1, always contains a slow component which is generally absent in the D2, T2 and T3 bursts; (iv) the peak flux is highest for S1, D1 and T1 bursts, but this is still a factor of 7 lower than the highest peak flux ever seen for a burst in this system; (v) the persistent flux, representing the mass accretion rate onto the neutron star, is about 1% of Eddington, which is among the lowest value so far measured for this system. The amount of energy per gram of accreted mass liberated during bursts is consistent with a fuel mixture of hydrogen-rich material. The characteristics of the bursts indicate that possibly all bursts in this system are hydrogen-ignited, in contrast with most other frequent X-ray bursters in which bursts are helium-ignited, but consistent with the low mass accretion rate in EXO 0748-676. Possibly the hydrogen ignition is the determining factor for the occurrence of short wait-time bursts. For example the 12 min wait time may be associated with a nuclear beta decay timescale. Appendix is only available in electronic form at http://www.aanda.org

The evolution of a complex solar radio burst corresponding to special configuration of microwave sources

A complex radio burst associated with periodic (∼1 and 6 min) pulsations and several kinds fine structures, e.g., normal- and reverse-drifting type III bursts, zebra patterns, and slowly drifting structure was observed with the radio spectrometers (1.0–2.0, 2.6–3.8, 5.2–7.6, and 0.65–1.5 GHz) at the National Astronomical Observatories of China (NAOC) in Beijing and Yunnan on 19 October 2001. In combination with the images of 17 and 34 GHz from NoRH and the magnetograms from MDI we reveal the existence and evolution of preexisting and new emerging sources, and find the horseshoe-shaped structure of microwave sources intensity during the late phase of the burst. Through the detailed comparison of the evolution of each source with the time profiles of radio bursts corresponding to these sources we indicate that the intimate correlation between the microwave sources evolution and the generation of the radio burst associated fine structures. Some fine structures can be considered as the MHD turbulence and plasma emission mechanism, based on the anisotropic beam instability and hybrid waves generations. From the characteristics of observations we may presume that the coronal magnetic structures should contain an extended coronal loop system and multiple discrete electrons acceleration/injection sites. The mechanisms of this complex radio burst are deal with the incoherent gyrosynchrotron emission from the trapped electrons and the coherent plasma emission from the non trapped electrons.

Microwave emission from the trapped and precipitated electrons in solar bursts

We analyzed the microwave spectra of a sample of 13 solar flares out of 40 events observed by the Nobeyama Radio Polarimeter in the period of August 8, 1998 through November 24, 2001. The solar burst time profiles were filtered to separate the slow component from the fast structures which were associated with the emission from trapped particles and to the emission from the minor precipitating population, respectively. The spectra of both components suggest a trap in a region with a mean magnetic field of about 600 G and a minor emission from the loop legs with a magnetic field of 1100 G, resulting in a mirror ratio of about two. The spectral indices of the optically thin emission from these two regions indicate pitch angle diffusion by Coulomb collisions.

Vector Nonlinear Time-Series Analysis of Gamma-Ray Burst Datasets on Heterogeneous Clusters

The simultaneous analysis of a number of related datasets using a single statistical model is an important problem in statistical computing. A parameterized statistical model is to be fitted on multiple datasets and tested for goodness of fit within a fixed analytical framework. Definitive conclusions are hopefully achieved by analyzing the datasets together. This paper proposes a strategy for the efficient execution of this type of analysis on heterogeneous clusters. Based on partitioning processors into groups for efficient communications and a dynamic loop scheduling approach for load balancing, the strategy addresses the variability of the computational loads of the datasets, as well as the unpredictable irregularities of the cluster environment. Results from preliminary tests of using this strategy to fit gamma-ray burst time profiles with vector functional coefficient autoregressive models on 64 processors of a general purpose Linux cluster demonstrate the effectiveness of the strategy.

Gamma‐Ray Burst Energetics and the Gamma‐Ray Burst Hubble Diagram: Promises and Limitations

We present a complete sample of 29 gamma-ray bursts (GRBs) for which it has been possible to determine temporal breaks (or limits) from their afterglow light curves. We interpret these breaks within the framework of the uniform conical jet model, incorporating realistic estimates of the ambient density and propagating error estimates on the measured quantities. In agreement with our previous analysis of a smaller sample, the derived jet opening angles of those 16 bursts with redshifts result in a narrow clustering of geometrically corrected gamma-ray energies about γ = 1.33 × 1051 ergs; the burst-to-burst variance about this value is 0.35 dex, a factor of 2.2. Despite this rather small scatter, we demonstrate in a series of GRB Hubble diagrams that the current sample cannot place meaningful constraints upon the fundamental parameters of the universe. Indeed, for GRBs to ever be useful in cosmographic measurements, we argue the necessity of two directions. First, GRB Hubble diagrams should be based upon fundamental physical quantities such as energy, rather than empirically derived and physically ill-understood distance indicators (such as those based upon prompt burst time-profiles and spectra). Second, a more homogeneous set should be constructed by culling subclasses from the larger sample. These subclasses, although now first recognizable by deviant energies, ultimately must be identifiable by properties other than those directly related to energy. We identify a new subclass of GRBs ("f-GRBs") that appear both underluminous by factors of at least 10 and exhibit a rapid fading (fν ∝ t-2) at early times (t ≲ 0.5 day). About 10%-20% of observed long-duration bursts appear to be f-GRBs.

The X-ray burst detected in 1991 from the transient source SAX J1747.0-2853

We present the observations of an intense X-ray burst from the recurrent transient source SAXJ1747.0-2853 located near the Galactic center. The burst was detected by the ART-P telescope onboard the Granat observatory on October 20, 1991. The burst time profile exhibits features that clearly point to an increase in the photospheric radius of the neutron star at the burst onset. This increase is attributable to an expansion of its outer hydrogen-rich atmospheric envelope under radiation pressure. After hydrogen-envelope outflow and photospheric contraction, the radiation flux emerging from deep within the star continued to rise, which several seconds later led to a recurrent, weaker photospheric expansion attributable to the outflow of the outer helium-envelope layers. Based on the described picture, we determined the distance to the source, d=7.9±0.4 kpc. No radiation was detected by the ART-P telescope from the source in quiescence. Actually, the source itself was discovered only seven years later by the BeppoSAX satellite during its X-ray activity.

Kerr black holes and time profiles of gamma ray bursts

The cumulative light curves of Gamma Ray Bursts (GRBs) smooth the spiky nature of the running light curve. The cumulative count increases in an approximate linear way with time t for most bursts. In 19 out of 398 GRBs with s, the cumulative light curve was found to increase with time as ~t2 implying a linear increase in the running light curve. The non-linear sections last for a substantial fraction of the GRB duration, have a large proportion of the cumulative count and many resolved pulses that usually end with the highest pulse in the burst. The reverse behaviour was found in 11 GRBs where the running light curve decreased with time and some bursts are good mirror images of the increases. These GRBs are among the spectrally hardest bursts observed by BATSE. The most likely interpretation is that these effects are signatures of black holes that are either being spun up or down in the accretion process. In the spin up case, the increasing Kerr parameter of the black hole allows additional rotational and accretion energy to become available for extraction. The process is reversed if the black hole is spun down by magnetic field torques. The luminosity changes in GRBs are consistent with the predictions of the BZ process and neutrino annihilation and thus provide the link to spinning black holes. GRBs provide a new window for studying the general relativistic effects of Kerr black holes.

IN SEARCH FOR NATURAL WORMHOLES

We have investigated 631 time profiles of gamma ray bursts from the BATSE database searching for observable signatures produced by microlensing events related to natural wormholes. The results of this first search of topologically nontrivial objects in the Universe can be used to constrain their number and mass.

Multiresolution analysis of solar mm–wave bursts

Two methods of multi-scale time series analysis are applied to solar mm-wavelength flux time profiles in order to assess the diagnostic power of these tools for the exploration of nonlinear energy release processes. Both the multiresolution analysis (MRA), a method based on the wavelet transform, and the structure function analysis (SFA) permit the treatment of non-stationary time series. In addition, the MRA offers a local decomposition of the scaling behavior of the flux variations. Our main emphasis is directed at a decomposition of the contributions of the different time scales to the overall flux profile. The methods yield consistent values of the spectral index which describes the scalings contained in the time series. We find that time profiles of bursts are qualitatively analogous to fractional Brownian motion (fBm), possessing long-range temporal correlations. Such correlations are not found in quiet Sun observations. The MRA of six solar mm-wave bursts shows that the radio flux is always composed of contributions from a broad range of time scales. Also during the main phase of bursts, which appears to be structurally analogous to the pre- and post-burst phases at a resolution limit of 1 s, flux fluctuations are enhanced in a broad range of time scales. This suggests that the mm-wave bursts are composed of unresolved elements, just as the pre- and post-burst time profiles. The underlying energy release thus appears to be fragmentary. These results are discussed in terms of the avalanche model and plasma physical models for solar energy release events.

Statistics of time histories and spectral variability of GRBs

We introduce new parameters for characterizing gamma-ray burst time profiles and energy spectra. Bursts with short and long duration T 90 are compared, and significant differences are found in the number of pulses and equivalent pulse widths. The trend of the average spectral parameters was resolved at the (α,E p) plane. The comparison between bright and dim bursts is done, which manifests the difference in the average emissivity curves and in the average spectral hardness.

Evidence for “Chain Reaction” in the Time Profiles of Gamma-Ray Bursts

Although the time profiles of gamma ray bursts (GRBs) show extremely diverse behavior, their average statistical properties such as the average peak-aligned profile and the auto-correlation function show simple stretched-exponential behavior. This could indicate that the diversity of all bursts is just due to different random realizations of the same simple stochastic process where the process is scale invariant in time. We illustrate how both the diversity of GRB time profiles and some important average statistical properties can be reproduced in this way using a simple toy model for a stochastic pulse avalanche, which behaves as a chain reaction in a near-critical regime. We suggest that one possibility for the underlying physical process for generating GRBs could be a chain detonation in which reconnecting magnetic turbulent features trigger each other.

Cosmological Evolution and Luminosity Function Effects on Number Counts, Redshift, and Time Dilation of Bursting Sources

We present analytic formulae for the integral number count distribution of cosmological bursting or steady sources valid over the entire range of fluxes, including density evolution and either standard candle or a power law luminosity function. These are used to derive analytic formulae for the mean redshift, the time dilations and the dispersion of these quantities for sources within a given flux range for Friedmann models with $\Omega=1,~ \Lambda=0$ without K-corrections, and we discuss the extension to cases with $\Omega <1$ and inclusion of K-corrections. Applications to the spatial distribution of cosmological gamma ray burst sources are discussed, both with and without an intrinsic energy stretching of the burst time profiles, and the implied ranges of redshift $z$ are considered for a specific time dilation signal value. The simultaneous consideration of time dilation information and of fits of the number distribution versus peak flux breaks the degeneracy inherent in the latter alone, allowing a unique determination of the density evolution index and the characteristic luminosity of the sources. For a reported time dilation signal of 2.25 and neglecting [including] energy stretching we find that the proper density should evolve more steeply with redshift than comoving constant, and the redshifts of the dimmest sources with stretching would be very large. However, the expected statistical dispersion in the redshifts is large, especially for power law luminosity functions, and remains compatible with that of distant quasars. For smaller time dilation values of 1.75 and 1.35 the redshifts are more compatible with conventional ideas about galaxy formation, and the evolution is closer to a comoving constant or a slower evolution. More generally, we have considered a wide range of possible measured time dilation

The Autocorrelation of Gamma-Ray Burst Time Profiles

The autocorrelation of time profiles of emission from gamma-ray bursts has previously been proved to be a valuable diagnostic for the study of the timing behavior of these bursts. In particular, comparative studies benefited from this diagnostic. However, in these previous studies, the particular shape of the autocorrelation function has not been addressed in great detail. In the present paper we try to explain the autocorrelation shape and behavior. We propose an empirical model that aids in the evaluation of uncertainties in autocorrelation analyses of gamma-ray burst time profiles. Our most important conclusions are that analyses based on the autocorrelation function are not dominated by mathematical properties not connected with the gamma-ray burst phenomenon, and that the uncertainty in the relative time stretching between different photon energy ranges found through such an analysis previously from {ital CGRO} BATSE data is less than or equal to 10{percent}. {copyright} {ital 1996 The American Astronomical Society.}

Decameter solar type III bursts: Data classification with use of cluster analysis

The many-parametric data on decametric type III bursts containing more than 1000 events were classified with use of cluster analysis, i.e., the pattern recognition procedure. For the classification such parameters have been used as intensity, duration and degree of circular polarization derived from burst time profiles. The automatic classification has resulted in division of daily samples of type III bursts into classes of bursts, more homogeneous statistically, which can be associated with different components of type III radiation distinguished by their physical origin. For the classes obtained, statistically reliable dependences of the mean intensity on source position can be found which allow one to conclude about the source structure and evolution, as well as about the characteristics defined by a burst generation mechanism and propagation effects.