The p-Laplacian as a Framework for Generalizing Newtonian Gravity and MoND
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2025
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| author | Scherer, D. Pflamm-Altenburg, J. Kroupa, P. Gjergo, E. |
| author_facet | Scherer, D. Pflamm-Altenburg, J. Kroupa, P. Gjergo, E. |
| contents | The Radial Acceleration Relation (RAR) follows from Milgromian gravitation (MoND). Velocity dispersion data of many dwarf spheroidal galaxies (dSphs) and galaxy clusters have been reported to be in tension with it. We consider the Generalized Poisson Equation (GPE), expressed in terms of the p-Laplacian, which has been applied in electrodynamics. We investigate whether it can address these tensions. From the GPE we derive a generalized RAR characterized by the $p$-parameter from the p-Laplacian and a velocity dispersion formula for a Plummer model. We apply these models to Milky Way and Andromeda dSphs and HIFLUGS galaxy clusters and derive a $p$-parameter for each dSph and galaxy cluster. We explore a relation of $p$ to the mass density of the bound system, and alternatively a relation of $p$ to the external field predicted from Newtonian gravity. This ansatz allows the deviations of dSphs and galaxy clusters from the RAR without introducing dark matter. Data points deviate from the Milgromian case, $p=3$, with up to $5σ$-confidence. Also, we find the model predicts velocity dispersions, each of which lies in the 1$σ$-range of their corresponding data point allowing the velocity dispersion to be predicted for dSphs from their baryonic density. The functional relation between the mass density of the bound system and $p$ suggests $p$ to increase with decreasing density. We find for the critical cosmological density $p(ρ_{\text{crit}}) = 12.27 \pm 0.39$. This implies significantly different behaviour of gravitation on cosmological scales. Alternatively, the functional relation between $p$ and the external Newtonian gravitational field suggests $p$ to decrease with increasing field strength. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_17002 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The p-Laplacian as a Framework for Generalizing Newtonian Gravity and MoND Scherer, D. Pflamm-Altenburg, J. Kroupa, P. Gjergo, E. Astrophysics of Galaxies The Radial Acceleration Relation (RAR) follows from Milgromian gravitation (MoND). Velocity dispersion data of many dwarf spheroidal galaxies (dSphs) and galaxy clusters have been reported to be in tension with it. We consider the Generalized Poisson Equation (GPE), expressed in terms of the p-Laplacian, which has been applied in electrodynamics. We investigate whether it can address these tensions. From the GPE we derive a generalized RAR characterized by the $p$-parameter from the p-Laplacian and a velocity dispersion formula for a Plummer model. We apply these models to Milky Way and Andromeda dSphs and HIFLUGS galaxy clusters and derive a $p$-parameter for each dSph and galaxy cluster. We explore a relation of $p$ to the mass density of the bound system, and alternatively a relation of $p$ to the external field predicted from Newtonian gravity. This ansatz allows the deviations of dSphs and galaxy clusters from the RAR without introducing dark matter. Data points deviate from the Milgromian case, $p=3$, with up to $5σ$-confidence. Also, we find the model predicts velocity dispersions, each of which lies in the 1$σ$-range of their corresponding data point allowing the velocity dispersion to be predicted for dSphs from their baryonic density. The functional relation between the mass density of the bound system and $p$ suggests $p$ to increase with decreasing density. We find for the critical cosmological density $p(ρ_{\text{crit}}) = 12.27 \pm 0.39$. This implies significantly different behaviour of gravitation on cosmological scales. Alternatively, the functional relation between $p$ and the external Newtonian gravitational field suggests $p$ to decrease with increasing field strength. |
| title | The p-Laplacian as a Framework for Generalizing Newtonian Gravity and MoND |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.17002 |