Numerical Simulations Reveal the Origin of QPOs in Black Hole Candidates

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dc.creatorChakrabarti, Sandip K.
dc.date2005-01-14
dc.date.accessioned2026-07-07T02:16:45Z
dc.date.available2026-07-07T02:16:45Z
dc.descriptionWe present results of various types of numerical simulations of black hole accretion disks and find that those flows which are relatively non-dissipative and which contain accretion shocks are the best candidates so far. The power density spectra (PDS) reveal the aspects which are similar to what are observed in black hole candidates.
dc.description6 pages, 7 figures To be published in the Proceedings of 5th Microquasar Conference (Beijing, 2004)
dc.identifierhttps://arxiv.org/abs/astro-ph/0501299
dc.identifierhttp://arxiv.org/abs/astro-ph/0501299
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8907
dc.subjectAstrophysics
dc.titleNumerical Simulations Reveal the Origin of QPOs in Black Hole Candidates
dc.typetext

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