SearcharxivSearch

arXiv · astro-ph/0507045

Relation between the hardness ratio and time in the first 2 seconds for compatible samples of short and long gamma-ray bursts

Abstract

In this paper, we randomly selected a sample (sample 1) of long gamma-ray bursts, with its size being the same as that of the short burst group (sample 2) (N=500), from the Current BATSE Bursts Catalog. We randomly selected a short burst and assigned its T90 to each of these long bursts. We thus constructed a long burst sample with both the sample size and the distribution of T90 being the same as those of the short burst sample obtained from the Current BATSE Bursts Catalog. Then we calculated the hardness ratio ($hr_{T}$) over the assigned T90 for the long bursts and over their own T90 for the shout bursts, and studied the relation between the hardness ratio and the corresponding T90 for these two samples. We also calculated the hardness ratio ($hr_{t}$) over the randomly selected 64 ms time intervals within the T90, and investigated the relation between this hardness ratio and the selected 64 ms time interval. In addition, the $hr_{t}$ within and beyond the first 2 seconds for all the long bursts (sample 3; N=1541) were also investigated. We found that the KS probabilities of the distributions of the $hr_{T}$ (7.15337E-15) and $hr_{t}$ (9.54833E-10) for samples 1 and 2 are very small, and the average value of $hr_{T}$ and $hr_{t}$ of short bursts are obviously larger than that of the long bursts. The correlations between log$hr_{T}$ and logT90, and between log$hr_{t}$ and log t, for samples 1 and 2 are different. These show that short and long bursts in the first 2 seconds have different characters and they probably originate from different progenitors. For sample 3, for the two time intervals, the KS probability is 5.35828E-5, which suggests that the hardness ratios in different time intervals for long bursts are also different.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Yi-Ping Qin, Yun-Ming Dong. 2005-07-02. Relation between the hardness ratio and time in the first 2 seconds for compatible samples of short and long gamma-ray bursts. https://doi.org/10.1111/j.1365-2966-2005.08794.x

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Dark Energy is the Cosmological Quantum Vacuum Energy of Light Particles-The Axion and the Lightest Neutrino

We uncover the general mechanism producing the dark energy(DE). This is only based on well known quantum physics and cosmology. We show that the observed DE originates from the cosmological quantum vacuum of light particles which provides a continuous energy distribution able to reproduce the data. Bosons give positive contributions to the DE while fermions yield negative contributions. As usual in field theory, ultraviolet divergences are subtracted from the physical quantities. The subtractions respect the symmetries of the theory and we normalize the physical quantities to be zero for the Minkowski vacuum. The resulting finite contributions to the energy density and the pressure from the quantum vacuum grow as log a(t) where a(t) is the scale factor, while the particle contributions dilute as 1/a^3(t), as it must be for massive particles. The DE equation of state P = w(z)H turns to be w(z)<-1 with w(z) asymptotically reaching the value -1 from below.A scalar particle can produce the observed DE through its quantum cosmological vacuum provided:(i)its mass is of the order of 10^{-3} eV = 1 meV,(ii) it is very weakly coupled and (iii) it is stable on the time scale of the age of the universe. The axion vacuum thus appears as a natural candidate. The neutrino vacuum (especially the lightest mass eigenstate) can give negative contributions to the DE. We find that w(z=0) is slightly below -1 by an amount ranging from [-1.5 10^{-3}] to [-8 10^{-3}] and we predict the axion mass to be in the range between 4 and 5 meV. We find that the universe will expand in the future faster than the de Sitter universe, as an exponential in the square of the cosmic time. DE arises from the quantum vacua of light particles in FRW cosmological space time in an analogous way to the Casimir effect in Minkowski spacetime with non trivial boundaries.

astro-ph

Scaling of Black Hole Accretion Discs from Gamma-Ray Bursts and Black Hole X-Ray Binaries to Active Galactic Nuclei

I consider how physical processes scale over eight orders of magnitude in black hole mass, from stellar masses in gamma-ray bursts (GRB) and black-hole X-ray binaries (BHXRB) to supermassive active galactic nuclei (AGN). Accretion rates onto stellar mass black holes range over more than sixteen orders of magnitude, from the lower luminosity BHXRB to GRB. These enormous parameter ranges correspond to qualitative as well as quantitative differences in behavior. The fundamental questions involve the balance between nonequilibrium and thermalized plasmas. When energy fluxes exceed a critical value $\sim 10^{29}$ erg/cm$^2$s, as in GRB, a black-body equilibrium pair plasma forms. At the lower fluxes found in AGN, BHXRB and microquasars, accretion power electrodynamically accelerates a small number of very energetic particles, explaining their non-thermal spectra and the high energy gamma-ray emission of blazars. Ultra-high energy cosmic rays may be accelerated by massive black holes, otherwise undetectable, with very low thermal luminosities. New-born fast high-field pulsars may be in the black-body equilibrium regime, resembling SGR in permanent outburst. I also consider the question, significant for the acceleration of nonthermal particles in GRB outflows, of whether collisionless plasmas interpenetrate rather than forming hydrodynamic shocks, and propose this as an alternative to internal shock models of GRB. A new appendix attempts to explain why AGN are, proportionally, more efficient accelerators of energetic particles than stellar mass black holes.

astro-ph