Cygnus X-1 light curve (counts and spectral hardness)

Cygnus X-1 is one of the best black hole candidates amongst massive X-ray binaries. An artist's conception of this source is available. This figure shows the lightcurve and spectral hardness of Cygnus X-1 on September 4, 1973 as collected by the Copernicus satellite. During the dip at 930.5 - 930.6, we see the spectral hardness increase relative to the quiescent state. The increased spectral hardness is most likely due to absorption of softer X-rays by some intervening matter.

In Cyg X-1, these dips usually occur at superior conjunction, the point where the large companion star passes more or less between us and the accreting black hole. The soft component of the spectrum might be associated with an accretion disk corona, while the hard component comes from the inner regions of the disk near the compact object. During the dips, some clumps or blobs of matter in the stellar wind of the supergiant or the outer area of the disk block, absorb or scatter some of the softer X-rays, causing an overall hardening of the spectrum.

Cygnus X-1 counts and hardness light curve

(Enter the object name)
Additions or Comments: Have we left anything out? Is there something you would like to have added to this page (a link to your own group's research page, for example...)?

IMAGES | By Mission | Stars | Cataclysmic Variables | X-ray Binaries | Pulsars | Supernova Remnants & Planetary Nebulae | Galaxies | Active Galactic Nuclei | Clusters and Groups of Galaxies | X-ray/gamma-ray Background & Deep Fields | Solar System Objects | Gamma Ray Bursts

HEASARC Home | Observatories | Archive | Calibration | Software | Tools | Students/Teachers/Public

Last modified: Thursday, 26-Jun-2003 13:48:45 EDT

HEASARC support for unencrypted FTP access ended on September 20, 2019. Please see this notice for details.