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Title:
QPO Evolution in 2005 Outburst of the Galactic Nano Quasar GRO J1655-40
Authors:
Debnath, D.; Nandi, A.; Pal, P. S.; Chakrabarti, S. K.
Affiliation:
AA(Indian Centre For Space Physics, 43 Chalantika, Garia Station Road, Kolkata 700084, India), AB(Indian Centre For Space Physics, 43 Chalantika, Garia Station Road, Kolkata 700084, India; On deputation from ISRO-HQ, New BEL Road, Bangalore, 560094), AC(Indian Centre For Space Physics, 43 Chalantika, Garia Station Road, Kolkata 700084, India), AD(S. N. Bose National Center for Basic Sciences, JD-Block, Salt Lake, Kolkata, 700098, India; Indian Centre For Space Physics, 43 Chalantika, Garia Station Road, Kolkata 700084, India)
Publication:
OBSERVATIONAL EVIDENCE FOR BLACK HOLES IN THE UNIVERSE: Proceedings of the 2nd Kolkata Conference on Observational Evidence for Black Holes in the Universe held in Kolkata India, 10-15 February 2008 and the Satellite Meeting on Black Holes, Neutron Stars, and Gamma-Ray Bursts held 16-17 February 2008. AIP Conference Proceedings, Volume 1053, pp. 171-175 (2008). (AIPC Homepage)
Publication Date:
10/2008
Origin:
AIP
PACS Keywords:
Binary and multiple stars, Galactic nuclei , circumnuclear matter, and bulges, Astronomical and space-research instrumentation
DOI:
10.1063/1.3009477
Bibliographic Code:
2008AIPC.1053..171D

Abstract

GRO J1655-40 showed significant X-ray activity in the last week of February, 2005 and remained active for the next 260 days. The rising and the decline phases of this particular outburst show evidence for systematic movements of the Componizing region, assumed to be a CENBOL, which causes the Quasi-periodic Oscillations or QPOs. We present both the spectral and the timing results of the RXTE/PCA data taken from these two hard spectral states. Assuming that the QPOs originate from an oscillating shock CENBOL, we show how the shock slowly moves in through the accretion flow during the rising phase at a constant velocity and accelerate away outward during the later part of the decline phase. By fitting the observed frequencies with our solution, we extract time variation of various disk parameters such as the shock locations, velocity etc.
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