تقرير
The baryonic-to-halo mass relation from mass and energy cascade in self-gravitating collisionless dark matter flow
| العنوان: | The baryonic-to-halo mass relation from mass and energy cascade in self-gravitating collisionless dark matter flow |
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| المؤلفون: | Xu, Zhijie (Jay) |
| سنة النشر: | 2022 |
| المجموعة: | Zenodo |
| مصطلحات موضوعية: | cosmology, dark matter, turbulence, simulation, astronomy, astrophysics, dark matter halo, correlation, statistical analysis, self-gravitating, collisionless, N body, mass cascade, energy cascade, baryonic-to-halo mass ratio, stellar-to-halo mass ratio |
| الوصف: | The baryonic-to-halo mass relation from mass and energy cascade in dark matter flow The relation between properties of galaxies and dark matter (DM) halos they reside in can be valuable to understand the structure formation and evolution. In particular, the baryonic-to-halo mass ratio (BHMR) and its evolution may provide many important insights. We first review unique properties of self-gravitating collisionless dark matter flow (SG-CFD), followed by their applications in deriving BHMR. To maximize system entropy, the long-range interaction requires a broad size of halos to be formed. These halos facilitate an inverse mass and energy cascade from small to large scales that involves a constant rate of energy cascade \(\varepsilon_u \approx -4.6\times 10^{-7} m^2/s^3\). The mass and energy cascade represent an intermediate statistically steady state of dark matter flow. In addition, dark matter flow exhibits scale-dependent flow behaviors that is incompressible on small scale and irrotational on large scale. Considering a given halo with a total baryonic mass \(m_b\), halo mass \(m_h\), halo virial size \(r_h\), and flat rotation speed \(v_f\), the baryonic-to-halo mass relation can be analytically derived by combining the baryonic Tully-Fisher relation and the rate of energy cascade \(\varepsilon_u\) in small and large halos. We found a maximum BHMR ratio ~0.076 for halos with a critical mass \(m_{hc}\sim 10^{12}M_{sun}\) at z=0. That ratio is much lower for both smaller and larger halos such that two regimes can be identified: i) for incompressible small halos with mass \(m_h |
| نوع الوثيقة: | report |
| اللغة: | English |
| العلاقة: | https://zenodo.org/record/6640355Test; https://doi.org/10.48550/arXiv.2203.06899Test; oai:zenodo.org:6640355 |
| DOI: | 10.48550/arXiv.2203.06899 |
| الإتاحة: | https://doi.org/10.48550/arXiv.2203.06899Test https://doi.org/10.5281/zenodo.6569901Test https://doi.org/10.5281/zenodo.6569898Test https://doi.org/10.5281/zenodo.6541230Test https://doi.org/10.5281/zenodo.6586212Test https://doi.org/10.48550/arXiv.2109.12244Test https://doi.org/10.48550/arXiv.2110.03126Test https://doi.org/10.48550/arXiv.2110.05784Test https://doi.org/10.48550/arXiv.2110.09676Test https://doi.org/10.48550/arXiv.2110.13885Test |
| حقوق: | info:eu-repo/semantics/openAccess ; https://creativecommons.org/licenses/by/4.0/legalcodeTest |
| رقم الانضمام: | edsbas.3FE6CE61 |
| قاعدة البيانات: | BASE |
| DOI: | 10.48550/arXiv.2203.06899 |
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