Shot model parameters for Cygnus X-1 through phase portrait fitting

Details Shot model parameters for Cygnus X-1 through phase portrait fitting Shot model parameters for Cygnus X-1 through phase portrait fitting

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...376..295l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 376, July 20, 1991, p. 295-311. DOE-supported research.

Statistics

Computation

61

Accretion Disks, Power Spectra, Shot Noise, Stellar Models, Variable Stars, X Ray Sources, Computational Astrophysics, Exosat Satellite, Heao 1, Spaceborne Astronomy

Scientific paper

Shot models for systems having about 1/f power density spectrum are developed by utilizing a distribution of shot durations. Parameters of the distribution are determined by fitting the power spectrum either with analytic forms for the spectrum of a shot model with a given shot profile, or with the spectrum derived from numerical realizations of trial shot models. The shot fraction is specified by fitting the phase portrait, which is a plot of intensity at a given time versus intensity at a delayed time and in principle is sensitive to different shot profiles. These techniques have been extensively applied to the X-ray variability of Cygnus X-1, using HEAO 1 A-2 and an Exosat ME observation. The power spectra suggest models having characteristic shot durations lasting from milliseconds to a few seconds, while the phase portrait fits give shot fractions of about 50 percent. Best fits to the portraits are obtained if the amplitude of the shot is a power-law function of the duration of the shot. These fits prefer shots having a symmetric exponential rise and decay. Results are interpreted in terms of a distribution of magnetic flares in the accretion disk.

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