2003/03/25 by V. A. Arefiev, Vadim A. Arefiev, W. Priedhorsky +3 · 27 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cosmic distance ladder #Gamma-ray burst #Gamma-ray bursts and supernovae #Luminosity #Luminosity function #Physics #Power law #Pulsars and Gravitational Waves Research #ROSAT #Sky #Statistics #astro-ph
paper · pdf · doi:10.1086/367761
published in The Astrophysical Journal 586(2), 1238-1249 (IOP Publishing) · 36 pages, 8 figures
openalex publication_date 2003/03/25 · arxiv created 2003/04/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Fast X-ray transients (FXTs) with timescales from seconds to hours have been seen by numerous space instruments. Because they occur at unpredictable locations, they are difficult to observe with narrow-field instruments. Only a few hundred have been detected, although their all-sky rate is in the tens of thousands per year. We have assembled archival data from Ariel-5 , HEAO 1 (A-1 and A-2), WATCH, ROSAT , and Einstein to produce a global fluence-frequency relationship for these events. Fitting the log N - log S distribution over several orders of magnitude to a simple power law, we find a slope of -1.0 . The sources of FXTs are undoubtedly heterogeneous, representing several physical phenomena; the α ~ -1 power law is an approximate result of the summation of these multiple sources. Two major contributions come from gamma-ray bursts and stellar flares. These two types of progenitors are distributed isotropically in the sky; however, their individual luminosity distributions are both flatter than the -3/2 power law that applies to uniformly distributed standard candles. Extrapolating from the BATSE catalog of gamma-ray bursts (GRBs), we find that the fraction of X-ray flashes that can be the X-ray counterparts of gamma-ray bursts is a function of fluence. The exact fraction of GRB-induced X-ray counterparts is sensitive to the R X/γ distribution, which we estimate from available experimental measurements. Certainly, most FXTs are not counterparts of standard gamma-ray bursts. The fraction of FXTs from non-GRB sources, such as magnetic stars, is greatest for the faintest FXTs. Our understanding of the FXT phenomenon remains limited and would greatly benefit from a large, homogeneous data set, which requires a wide-field, sensitive instrument.