The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE

Author:

Zhang Yuexin1ORCID,Méndez Mariano1,García Federico12ORCID,Karpouzas Konstantinos13ORCID,Zhang Liang43ORCID,Liu Honghui5,Belloni Tomaso M6,Altamirano Diego3

Affiliation:

1. Kapteyn Astronomical Institute, University of Groningen , PO BOX 800, 9700 AV Groningen, the Netherlands

2. Instituto Argentino de Radioastronomía (CCT La Plata, CONICET; CICPBA; UNLP) , C.C.5, (1894) Villa Elisa, Buenos Aires, Argentina

3. School of Physics and Astronomy, University of Southampton , Southampton SO17 1BJ, UK

4. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , Beijing 100049, People’s Republic of China

5. Center for Field Theory and Particle Physics and Department of Physics, Fudan University , 200438 Shanghai, China

6. INAF - Osservatorio Astronomico di Brera , via E. Bianchi 46, I-23807 Merate, Italy

Abstract

ABSTRACT GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30–150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the χ class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anticorrelated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1–2 per cent at ∼3 keV to ∼10–15 per cent at ∼30 keV. We suggest that the bump and the HFQPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft γ class, or to a bump when the spectrum is in the hard χ class. Finally, we discuss the anticorrelation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.

Funder

China Scholarship Council

NWO

CONICET

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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