The pre-outburst flare of the A0535+26 August/September 2005 outburst
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The pre-outburst flare of the A0535+26 August/September 2005 outburst

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The pre-outburst flare of the A0535+26 August/September 2005 outburst

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dc.contributor.author Caballero, I.
dc.contributor.author Santangelo, A.
dc.contributor.author Kretschmar, P.
dc.contributor.author Staubert, R.
dc.contributor.author Postnov, K.
dc.contributor.author Klochkov, D.
dc.contributor.author Camero Arranz, Ascensión
dc.contributor.author Finger, M. H.
dc.contributor.author Kreykenbohm, I.
dc.contributor.author Pottschmidt, K.
dc.contributor.author Rothschild, R. E.
dc.contributor.author Suchy, S.
dc.contributor.author Wilms, J.
dc.contributor.author Wilson, C. A.
dc.date.accessioned 2010-07-13T08:15:50Z
dc.date.available 2010-07-13T08:15:50Z
dc.date.issued 2008
dc.identifier.uri http://hdl.handle.net/10550/16003
dc.description.abstract Aims. We study the spectral and temporal behavior of the High Mass X-ray Binary A 0535+26 during a “pre-outburst flare” which took place ∼5 d before the peak of a normal (type I) outburst in August/September 2005. We compare the studied behavior with that observed during the outburst. Methods. We analyse RXTE observations that monitored A 0535+26 during the outburst. We complete spectral and timing analyses of the data. We study the evolution of the pulse period, present energy-dependent pulse profiles both at the initial pre-outburst flare and close to outburst maximum, and measure how the cyclotron resonance-scattering feature (hereafter CRSF) evolves. Results. We present three main results: a constant period P = 103.3960(5) s is measured until periastron passage, followed by a spin-up with a decreasing period derivative of P ̇ = (−1.69 ± 0.04) × 10−8 s s−1 at MJD 53 618, and P remains constant again at the end of the main outburst. The spin-up provides evidence for the existence of an accretion disk during the normal outburst. We measure a CRSF energy of Ecyc ∼ 50 keV during the pre-outburst flare, and Ecyc ∼ 46 keV during the main outburst. The pulse shape, which varies significantly during both pre-outburst flare and main outburst, evolves strongly with photon energy. en
dc.language.iso en en
dc.relation http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361:20079310&Itemid=129 en
dc.source Caballero, I., Santangelo, A., Kretschmar, P., Staubert, R., Postnov, K., Klochkov, D., Camero Arranz, A., Finger, M. H., Kreykenbohm, I., Pottschmidt, K., Rothschild, R. E., Suchy, S., Wilms, J. and Wilson, C. A. (2008): The pre-outburst flare of the A0535+26 August/September 2005 outburst, Astronomy and Astrophysics, núm. 480, vol. 2, pp. L17-L20 en
dc.subject X-rays : binaries; Stars : magnetic fields; Stars : individual : A 0535+26 en
dc.title The pre-outburst flare of the A0535+26 August/September 2005 outburst en
dc.type info:eu-repo/semantics/article en
dc.type info:eu-repo/semantics/publishedVersion en
dc.subject.unesco UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia::Estrellas en
dc.subject.unesco UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia::Fuentes de Rayos X en
dc.identifier.doi 10.1051/0004-6361:20079310 en
dc.description.private ascension.camero@uv.es en

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