X-Ray Pulsations from Cygnus X-1 Observed from UHURU

Oda, M.; Gorenstein, P.; Gursky, H.; Kellogg, E.; Schreier, E.; Tananbaum, H.; Giacconi, R.

doi:10.1086/180726

Cited by 157 publications

(55 citation statements)

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“…The observation by UHURU of rapid variability in Cyg X-1 reported by Oda [15] was soon followed by the rocket flights of the GSFC and MIT groups. These observations clarified that the observed pulsations were not periodic but chaotic.…”

Section: The Binary X-ray Sourcesmentioning

confidence: 93%

The Dawn of X‐Ray Astronomy (Nobel Lecture)

Giacconi

2003

ChemPhysChem

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Riccardo Giacconi joined the American Science and Engineering Corporation (AS & E) after leaving Princeton University in 1959, and in 1962 his group there detected the first extrasolar Xray source. Prof. Giacconi was subsequently responsible for the launch and use of the satellite UHURU (1970) and the EINSTEIN observatory (1978). He was appointed Associate Director of the High Energy Astrophysics Division of the Harvard‐Smithsonian Center for Astrophysics in 1973 and was also appointed Professor of Astronomy at Harvard University that same year. In 1981 he became the first Director of the Space Telescope Science Institute and was also appointed Professor in the Department of Physics and Astronomy at Johns Hopkins University. In 1992 he was appointed Director General of the European Southern Observatory, an intergovernmental organization of eight nations. Prof. Giaconni is currently President of Associated Universities, Inc., and Research Professor at Johns Hopkins University. He was awarded the Wolf Prize in 1987, and the Nobel Prize for Physics in 2002.

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Section: The Binary X-ray Sourcesmentioning

confidence: 93%

The Dawn of X‐Ray Astronomy (Nobel Lecture)

Giacconi

2003

ChemPhysChem

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“…Aperiodic variability in the X-ray flux of accreting sources was discovered at the dawn of X-ray astronomy (e.g., Oda et al 1971) and since then it has been extensively studied, mostly in the frequency domain, through the use of Fourier analysis techniques (van der Klis 1989). The noise power spectrum in accreting sources has been shown to follow a power law in broad range of frequencies.…”

Section: Aperiodic X-ray Flux Variations As a Tool To Measure Ns Magnmentioning

confidence: 99%

Magnetic Fields of Neutron Stars in X-Ray Binaries

Revnivtsev

Mereghetti

2016

Space Sciences Series of ISSI

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A substantial fraction of the known neutron stars resides in X-ray binaries -systems in which one compact object accretes matter from a companion star. Neutron stars in X-ray binaries have magnetic fields among the highest found in the Universe, spanning at least the range from ∼ 10 8 to several 10 13 G. The magnetospheres around these neutron stars have a strong influence on the accretion process, which powers most of their emission. The magnetic field intensity and geometry, are among the main factors responsible for the large variety of spectral and timing properties observed in the X-ray energy range, making these objects unique laboratories to study the matter behavior and the radiation processes in magnetic fields unaccessible on Earth. In this paper we review the main observational aspects related to the presence of magnetic fields in neutron star X-ray binaries and some methods that are used to estimate their strength.

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“…This optical object shows a binary nature, even though no such behaviour has been clearly seen in the X-ray region. The suggestion by Oda et al (1971) that a pulsating periodicity exists in the X-ray emission resulted in several observations about short-time variability, even though the pulsating periodicity has not been confirmed. The observation of the short time variability suggests a compact source, which together with the mass estimates for the X-ray source leads to the possibility of it being a 'black hole'.…”

Section: Iii31 X-ray Observationsmentioning

confidence: 99%

“…Oda et al (1971), using observations of the X-ray instrument in UHURU found that Cyg X-1 showed pulsations occurring several times a second and with less than a fraction of a second duration. The amplitude of the pulsations was at times more than 25 per cent of the average intensity.…”

Section: Iii31 X-ray Observationsmentioning

confidence: 99%