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A physical process of the radial acceleration of disc galaxies

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Wilhelm,  Klaus
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

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Citation

Wilhelm, K., & Dwivedi, B. N. (2018). A physical process of the radial acceleration of disc galaxies. Monthly Notices of the Royal Astronomical Society, 474(4), 4723-4729. doi:10.1093/mnras/stx2925.


Cite as: http://hdl.handle.net/21.11116/0000-0000-4330-E
Abstract
An impact model of gravity designed to emulate Newton's law of gravitation is applied to the radial acceleration of disc galaxies. Based on this model (Wilhelm et al. 2013), the rotation velocity curves can be understood without the need to postulate any dark matter contribution. The increased acceleration in the plane of the disc is a consequence of multiple interactions of gravitons (called ‘quadrupoles’ in the original paper) and the subsequent propagation in this plane and not in three-dimensional space. The concept provides a physical process that relates the fit parameter of the acceleration scale defined by McGaugh et al. (2016) to the mean free path length of gravitons in the discs of galaxies. It may also explain the gravitational interaction at low acceleration levels in MOdification of the Newtonian Dynamics (MOND, Milgrom 1983, 1994, 2015, 2016). Three examples are discussed in some detail: the spiral galaxies NGC 7814, NGC 6503 and M 33.