distance: 2.5 kpc
  • Granada 2000, Proceedings Microquasar Workshop, Granada 2000
  • Spiral image, Dying Pulse Train - Trick
  • Nuclear Physics B (Proc. Suppl.) 69 (1998) The Active X-Ray Sky : Results from Bepposax and Rxte : Proceedings of the Active X-Ray Sky, October 21-24, 1997, Rome, Italy, by L. Scarsi (Editor), H. Bradt (Editor), P. Giommi (Editor), F. Fiore (Editor), Elsevier Science 1998; ISBN: 0444829903
  • Chandra first light images
  • RXTE Rossi X-ray Timing Explorer (30.12.1995 Delta-II, 2-250 keV, PCA=proprotional count array, HEXTE=high energy X-ray timing experiment)
  • Periodic Time Variability Survey of ROSAT fields
  • BLACK HOLES IN BINARIES AND GALACTIC NUCLEI their Diagnostics, Demography, and Formation
  • ROSAT Service Area (including ROSAT Result Archive), XUV Center, An intermediate state of Cyg X-1, Galeev, Rossner, Vaiana: Structured Coronae of Accretion Disk, ApJ 229 (1979) 318-326, Modeling The Time Variability of Accreting Compact Sources
  • XEUS, 2000+: 6 m2, 0.1-30 keV, 2 to 5 arcsec at 1 keV, 10-18 erg/cm2/s
  • ABRIXAS, Astrophysikalisches Institut Potsdam. Start in Kapustin Yar bei Volgograd. Orbitale Parameter
  • virtual relativity
  • Modell
  • Marco, Valeri P. Frolov
  • Michael Mesterton-Gibbons, Mathematical Modelling
  • Time Series Analysis
  • Diss
  • Shot noise & Cyg X-1
  • Black Holes Signature From Advective Disks, A Big Black Hole Floats By
  • Living Reviews

    Die Quellen des sanften Roentgenschimmers (Astronomie)

    Der Weltraum glitzert und funkelt. Nicht nur wegen der Sterne oder der Hintergrundstrahlung. Sogar im Roentgenlicht erstrahlt er sanft in allen Richtungen. Was bislang als ein unerklaerliches diffuses Leuchten die Astronomen verwirrt hat, entpuppt sich bei genauerer Betrachtung mit dem Satelliten Chandra als Leuchtfeuer von unzaehligen Schwarzen Loechern, die ueber den ganzen Himmel verstreut sind. Einige davon sind so weit entfernt, dass wir von ihnen bislang kein Licht im sichtbaren Spektralbereich empfangen haben.

    Specific questions to be adressed are: 1. The origin of the hard X-ray spectra in Active Galactic Nuclei and galactic Black Hole Candidates. 2. The origin of the strong time variability observed in almost all accreting compact objects. There are many forms of Variability (over a large range of time scales) and one can not expect to explain all of them with a single model since their causes may be very different. Main targets are those forms of variability that are related directly to the formation of the X-ray spectrum, and those that have their origin in the interaction between the accretion disk and the magnetosphere of the accreting object. 3. The conditions that regulate the production of a jet by a compact object or protostar.

    Global theory of Balbus-Hawley instability
    According to the Rayleigh criterion hydrodynamic turbulence does not arise in Keplerian disks. Although magnetic fields are known to suppress the turbulence, numerical supercomputer experiments more and more reveal a magnetic origin of the turbulent instability. With the well-known formulations of dynamo theory we have computed the relevant amplitude of the magnetic fields in order to produce the turbulence. Only the interplay of non rigid rotation and (weak) magnetic field causes the desired instability.

    X-ray astronomy: Peeking into the obscured Universe

    GÜNTHER HASINGER: Observations with the sharpest X-ray eye available have started to unravel the mysteries of the cosmic X-ray background. The first images in the higher energy 'hard' X-ray range have helped resolve at least 75% of the background sources.

    Nature 404, 459 - 464 (2000)
    Resolving the extragalactic hard X-ray background

    The origin of the hard (2-10 keV) X-ray background has been a mystery for over 35 years. Most of the soft X-ray background has been resolved into individual sources (mainly quasars), but these sources do not have the spectral energy distribution required to match the spectrum of the X-ray background as a whole. Here we report the results of a deep survey, using the Chandra satellite, in which the detected hard X-ray sources account for at least 75 per cent of the hard X-ray background. The mean X-ray spectral energy distribution of these sources is in good agreement with that of the background. Moreover, most of those hard X-ray sources are associated unambiguously with either the nuclei of otherwise normal bright galaxies, or with optically faint sources. The latter could be active nuclei in dust-enshrouded galaxies or a population of quasars at extremely high redshift.



    RXTE GOF: Archives
    RXTE GOF: ASM Data Products
    MIT X-Ray Timing Explorer Project
    Argus: 3.5.2
    Argus Search Results of 4/11/00
    XANADU Software Home Page
    HEASARC Software
    RXTE GOF: Data Analysis & Processing
    RXTE GOF: Data Reduction and Analysis
    Directory of /xte/data/archive/AO1
    New Century of X-ray Astronomy, March 6-8, 2001, Yokohama, Japan
    Similarities and Universality in Relativistic Flows, SURF 2000, Mykonos, Greece, October 1-5, 2000

    The short timescale bursts of Cyg X-1 in the high and transitional states, Feng Yu-xin, Chen Li, Li Ti-pei, Chinese Astronomy and Astrophysics 23 1999 423 -- 434

    The X-ray power density spectrum of Cyg X-1 C. Li, F. Yu-xin, L. Ti-pei, L. Zong-wei, Chinese Astronomy and Astrophysics 24 2000 pp 159-168

    The radial temperature profile in the inner region of a black-hole accretion disk, Ding-xiong Wang, Chinese Astronomy and Astrophysics 24 2000 13 -- 22

    Wind driven accretion
    Wind driven accretion

    Didier BARRET Hard X-ray Emission From Low-Mass X-ray Binaries

    HETE-2 Mission


    IAU Symposium No.214: High Energy Processes and Phenomena in Astrophysics, 5-10 August, 2002 Suzhou, China

    Chinese Astronomy and Astrophysics Volume 25, Issue 4
    The time lag of high-energy photons of Cyg X-1 in hard state J.-l. Qu, T.-p. Li pp 416-424

    The time lag between hard and soft X-rays is an important aspect of the study of high-energy emission. Fourier cross spectrum, often used in calculating the time lag, is unable to measure statistically significant fast light variation above Fourier frequency 30 Hz from the measurements of Cyg X-1. The method of cross correlation function in time domain, developed by Li Ti-pei, can be effectively used in measuring time lags on different time scales. Using Li's method we discuss the properties of the time lag of high-energy photons of Cyg X-1 in hard state at different times. The results show that there is a significant time lap on short times scales (< 0.1 s). We confront different models of hard-state Cygnus X-1 with the observed time lag.