Numerical evolution of self-gravitating halos of self-interacting dark matter
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866912414373511168 |
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| author | Kamionkowski, Marc Sigurdson, Kris Slone, Oren |
| author_facet | Kamionkowski, Marc Sigurdson, Kris Slone, Oren |
| contents | We discuss a modification of a recently developed numerical scheme for evolving spherically symmetric self-gravitating systems to include the effects of self-interacting dark matter. The approach is far more efficient than traditional N-body simulations and cross sections with different dependencies on velocity and scattering-angle are easily accommodated. To demonstrate, we provide results of a simulation, which runs quickly on a personal computer, that shows the expected initial flattening of the inner region of an NFW halo as well as the later gravothermal collapse instability that leads to a dense core at the galactic center. We note that this approach can also be used, with some augmentation, to simulate the dynamics in globular clusters by modeling gravitational hard scattering as a self-interaction. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2506_04334 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Numerical evolution of self-gravitating halos of self-interacting dark matter Kamionkowski, Marc Sigurdson, Kris Slone, Oren Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies High Energy Physics - Phenomenology High Energy Physics - Theory 85A05, 85-08, 83C56, 82C22, 81V25 We discuss a modification of a recently developed numerical scheme for evolving spherically symmetric self-gravitating systems to include the effects of self-interacting dark matter. The approach is far more efficient than traditional N-body simulations and cross sections with different dependencies on velocity and scattering-angle are easily accommodated. To demonstrate, we provide results of a simulation, which runs quickly on a personal computer, that shows the expected initial flattening of the inner region of an NFW halo as well as the later gravothermal collapse instability that leads to a dense core at the galactic center. We note that this approach can also be used, with some augmentation, to simulate the dynamics in globular clusters by modeling gravitational hard scattering as a self-interaction. |
| title | Numerical evolution of self-gravitating halos of self-interacting dark matter |
| topic | Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies High Energy Physics - Phenomenology High Energy Physics - Theory 85A05, 85-08, 83C56, 82C22, 81V25 |
| url | https://arxiv.org/abs/2506.04334 |