2 Years ofINTEGRALMonitoring of GRS 1915+105. I. Multiwavelength Coverage withINTEGRAL,RXTE, and the Ryle Radio Telescope
| Autor: | Peggy Varniere, Osmi Vilhu, M. Tagger, M. Cadolle Bel, S. E. Shaw, Stephane Corbel, Peter Kretschmar, I. F. Mirabel, J. L. Rodriguez, A. Paizis, Jérôme Chenevez, C. Cabanac, Guy G. Pooley, Harry Lehto, T. M. Belloni, Diana Hannikainen |
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| Rok vydání: | 2008 |
| Předmět: |
Physics
010308 nuclear & particles physics Hardness ratio Astrophysics::High Energy Astrophysical Phenomena Radio flux Astronomy and Astrophysics Astrophysics Light curve Lambda 01 natural sciences Accretion (astrophysics) law.invention Radio telescope Amplitude Space and Planetary Science law 0103 physical sciences 010303 astronomy & astrophysics Flare |
| Zdroj: | The Astrophysical Journal. 675:1436-1448 |
| ISSN: | 1538-4357 0004-637X |
| DOI: | 10.1086/527369 |
| Popis: | (Abridged) We report the results of monitoring observations of the Galactic microquasar GRS 1915+105 performed simultaneously with INTEGRAL and RXTE Ryle . We present the results of the whole \integral campaign, report the sources that are detected and their fluxes and identify the classes of variability in which GRS 1915+105 is found. The accretion ejection connections are studied in a model independent manner through the source light curves, hardness ratio, and color color diagrams. During a period of steady ``hard'' X-ray state (the so-called class chi) we observe a steady radio flux. We then turn to 3 particular observations during which we observe several types of soft X-ray dips and spikes cycles, followed by radio flares. During these observations GRS 1915+105 is in the so-called nu, lambda, and beta classes of variability. The observation of ejections during class lambda are the first ever reported. We generalize the fact that a (non-major) discrete ejection always occurs, in GRS 1915+105, as a response to an X-ray sequence composed of a spectrally hard X-ray dip terminated by an X-ray spike marking the disappearance of the hard X-ray emission above 18 keV. We also identify the trigger of the ejection as this X-ray spike. A possible correlation between the amplitude of the radio flare and the duration of the X-ray dip is found in our data. In this case the X-ray dips prior to ejections could be seen as the time during which the source accumulates energy and material that is ejected later. |
| Databáze: | OpenAIRE |
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