314 citations · 5.3k across the 121 of their papers we have counts for
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No observational proof of the black-hole event-horizon
Marek A. Abramowicz, Wlodek Kluzniak, Jean-Pierre Lasota
Recently, several ways of obtaining observational proof of the existence of black-hole horizons have been proposed. We argue here that such proof is fundamentally impossible: obser…
An unusually low mass of some "neutron" stars?
D. Gondek-Rosinska, W. Kluzniak, N. Stergioulas
The X-ray emission of RXJ1856.5-3754 has been found to coincide to unprecedented accuracy with that of a blackbody, of radius 5.8+-0.9 km for the measured parallax distance of 140…
Epicyclic orbital oscillations in Newton's and Einstein's dynamics
Marek A. Abramowicz, Wlodek Kluzniak
We apply Feynman's principle, ``The same equations have the same solutions'', to Kepler's problem and show that Newton's dynamics in a properly curved 3-D space is identical with t…
The swallowing of a quark star by a black hole
Wlodzimierz Kluzniak, William H. Lee
In 3-d SPH simulations of the coalescence of a quark star with a pseudo-Newtonian black hole all of the quark matter is quickly accreted by the black hole. The Madsen-Caldwell-Frie…
Parametric epicyclic resonance in black hole disks: QPOs in micro-quasars
W. Kluzniak, M. A. Abramowicz
Non-linear acoustic coupling of modes in accretion disks allows a parametric resonance between epicyclic motions. In black hole disks, such a resonance first occurs, and is stronge…
Population synthesis of compact objects: neutron stars, strange (quark) stars and black holes
Krzysztof Belczynski, Tomasz Bulik, Wlodzimierz Kluzniak
We compute and present the distribution in mass of single and binary neutron stars, strange stars, and black holes. The calculations were performed using a stellar population synth…
Binary coalescence of a strange star with a black hole: Newtonian results
William H. Lee, Wlodzimierz Kluzniak, Jon Nix
We present Newtonian three-dimensional hydrodynamical simulations of the merger of quark stars with black holes. The initial conditions correspond to non-spinning stars in Kepleria…