0000000000208625

AUTHOR

Rüdiger Staubert

showing 3 related works from this author

A 0535+26 in the August/September 2005 outburst observed by RXTE and INTEGRAL

2007

In this Letter we present results from INTEGRAL and RXTE observations of the spectral and timing behavior of the High Mass X-ray Binary A 0535+26 during its August/September 2005 normal (type I) outburst with an average flux F(5-100keV)~400mCrab. The search for cyclotron resonance scattering features (fundamental and harmonic) is one major focus of the paper. Our analysis is based on data from INTEGRAL and RXTE Target of Opportunity Observations performed during the outburst. The pulse period is determined. X-ray pulse profiles in different energy ranges are analyzed. The broad band INTEGRAL and RXTE pulse phase averaged X-ray spectra are studied. The evolution of the fundamental cyclotron …

Astrophysics::High Energy Astrophysical PhenomenaCyclotronCyclotron resonanceFluxFOS: Physical sciencesAstrophysicsUNESCO::ASTRONOMÍA Y ASTROFÍSICAAstrophysicsSpectral linelaw.inventionlawX-raysLine (formation)PhysicsScatteringAstrophysics (astro-ph)Astronomy and AstrophysicsIndividual StarStars:ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO]Pulse (physics)X-rays ; binaries ; Stars ; Magnetic fields ; Individual Star ; A0535+26A0535+26Space and Planetary ScienceMagnetic fieldsHarmonicUNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogoniabinaries:ASTRONOMÍA Y ASTROFÍSICA [UNESCO]
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INTEGRAL/RXTE Observations of Cygnus X-1

2003

We present first results from contemporaneous observations of Cygnus X-1 with INTEGRAL and RXTE, made during INTEGRAL's performance verification phase in 2002 November and December. Consistent with earlier results, the 3-250 keV data are well described by Comptonization spectra from a Compton corona with a temperature of kT~50-90 keV and an optical depth of tau~1.0-1.3 plus reflection from a cold or mildly ionized slab with a covering factor of Omega/2pi~0.2-0.3. A soft excess below 10 keV, interpreted as emission from the accretion disk, is seen to decrease during the 1.5 months spanned by our observations. Our results indicate a remarkable consistency among the independently calibrated de…

Black hole physics ; Individual stars ; Cyg X-1 ; Gamma rays ; X-rays observations ; BinariesAstrophysics::High Energy Astrophysical PhenomenaPhase (waves)FOS: Physical sciencesFlux02 engineering and technologyAstrophysicsUNESCO::ASTRONOMÍA Y ASTROFÍSICAAstrophysicsCyg X-101 natural sciencesOmegaSpectral lineIonizationIndividual stars0103 physical sciencesOptical depth (astrophysics)0202 electrical engineering electronic engineering information engineeringCalibration010303 astronomy & astrophysicsOptical depthPhysics010308 nuclear & particles physicsGamma raysBinariesAstrophysics (astro-ph)X-rays observationsGamma rayAstronomyAstronomy and Astrophysics020206 networking & telecommunicationsBlack hole physics:ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO]CoronaSpace and Planetary ScienceReflection (physics)020201 artificial intelligence & image processingUNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia:ASTRONOMÍA Y ASTROFÍSICA [UNESCO]AIP Conference Proceedings
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X-Ray Spectral Variability of 3C273

1985

3C273 has been monitored by EXOSAT over the period December 1983 to June 1984 in 4 observations. In the December observation the flux was high and the spectrum showed a power law index of 1.5 changing to 0.9 at~8 keV. In subsequent observations the flux dropped to~40% of its original value and the hard tail disappeared. In the last observation the LE flux increased by a factor of 2 with no accompanying ME flux increase.

PhysicsSpectral indexX-ray astronomyX-rayCompton scatteringAstronomyFluxQuasarAstrophysicsPower lawX ray spectra
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