Spiral galaxy rotation curves determined from Carmelian general relativity

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dc.creatorHartnett, John G.
dc.date2005-11-28
dc.date2006-08-26
dc.date.accessioned2026-07-07T06:45:23Z
dc.date.available2026-07-07T06:45:23Z
dc.descriptionEquations of motion, in cylindrical co-ordinates, for the observed rotation of gases within the gravitational potential of spiral galaxies have been derived from Carmeli's Cosmological General Relativity theory. A Tully-Fisher type relation results and rotation curves are reproduced without the need for non-baryonic halo dark matter. Two acceleration regimes are discovered that are separated by a critical accleration $\approx 4.75 \times 10^{-10}$ $m.s^{-2}$. For accelerations larger than the critical value the Newtonian force law applies, but for accelerations less than the critical value the Carmelian regime applies. In the Newtonian regime the accelerations fall off as $r^{-2}$, but in the Carmelian regime the accelerations fall off as $r^{-1}$. This is new physics but is exactly what is suggested by Migrom's phenomenological MOND theory.
dc.description9 pages, 10 figures, Int. J. Theor. Phys, corrected typos
dc.identifierhttps://arxiv.org/abs/astro-ph/0511756
dc.identifierhttp://arxiv.org/abs/astro-ph/0511756
dc.identifierInt.J.Theor.Phys. 45 (2006) 2118-2136
dc.identifierdoi:10.1007/s10773-006-9178-0
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/103028
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleSpiral galaxy rotation curves determined from Carmelian general relativity
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