论文标题
从质量和能量级联质量级别的重质质量关系中，无碰撞的暗物质流量
The baryonic-to-halo mass relation from mass and energy cascade in self-gravitating collisionless dark matter flow
论文作者
论文摘要
它们所在的星系性能与暗物质光环之间的关系对于结构形成和进化可能是有价值的。本文重点介绍了重 - 升值质量比（BHMR）及其进化。我们首先回顾了自我磨碎的无碰撞暗物质流量（SG-CFD）的独特特性，然后将其应用于推导BHMR。为了最大程度地提高系统熵，远程相互作用需要形成较大的光晕。这些光晕促进了从小到大尺度的逆质量和能量级联，并以恒定的能量级联速率$ \ varepsilon_u $ $。此外，暗物质流动表现出与规模相关的流动行为，这些行为在小规模上是不可压缩的，并且在大规模上无关。有了这些属性，并考虑了给定的halo，带有总重质质量$ m_b $，halo mass $ m_h $，halo病毒尺寸$ r_h $以及平坦的旋转速度$ v_f $，可以通过将Baryonic tully-fisher关系和常量$ \ varepsilon_u $组合来分析得出BHMR。对于临界质量$ m_ {hc} \ sim 10^{12} m _ {\ odot} $，在z = 0时发现了最大BHMR比率〜0.076。对于较小和较大的光晕，该比率要低得多，因此可以识别两个方案：i）对于不可压缩的小晕圈，质量$ m_h <m_ <m_ {hc} $，我们有$ \ varepsilon_u \ propto v_f/r_h $，$ v_f \ propto r_h $，以及$ m_b \ prop prop propto propto propto propto propto propto propto propto propto propto propto m_h^4/3^4/3 ii）对于带质量$ m_h> m_h> m_h> m_h> m_h> m_h} $的大晕圈，我们有$ \ varepsilon_u \ propto v_f^3/r_h $，$ v_f \ propto r_h^{1/3} $，和$ m_b \ m_b \ m_b \ propto m_h^^4/9} $。结合双$ $λ$光晕质量函数，可以分析得出所有光环中的平均BHMR比（z = 0时〜0.024），以及其红移的演变。在z = 0时，所有星系中总重子的分数为〜7.6％，并且随时间$ \ propto t^{1/3} $增加。使用175个晚期星系的SPARC（Spitzer光度法\＆精确的旋转曲线）用于推导和比较。
The relation between properties of galaxies and dark matter halos they reside in can be valuable for structure formation and evolution. This paper focus on the baryonic-to-halo mass ratio (BHMR) and its evolution. We first review unique properties of self-gravitating collisionless dark matter flow (SG-CFD), followed by their application to derive BHMR. To maximize system entropy, the long-range interaction requires a broad size of halos to be formed. These halos facilitate inverse mass and energy cascade from small to large scales with a constant rate of energy cascade $\varepsilon_u$. In addition, dark matter flow exhibits scale-dependent flow behaviors that is incompressible on small scale and irrotational on large scale. With these properties and considering a given halo with a total baryonic mass $m_b$, halo mass $m_h$, halo virial size $r_h$, and flat rotation speed $v_f$, BHMR can be analytically derived by combining the baryonic Tully-Fisher relation and constant $\varepsilon_u$ in small and large halos. A maximum BHMR ratio ~0.076 is found for halos with a critical mass $m_{hc}\sim 10^{12}M_{\odot}$ 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 $m_h<m_{hc}$, we have $\varepsilon_u\propto v_f/r_h$, $v_f\propto r_h$, and $m_b\propto m_h^{4/3}$; ii) for large halos with mass $m_h>m_{hc}$, we have $\varepsilon_u\propto v_f^3/r_h$, $v_f\propto r_h^{1/3}$, and $m_b\propto m_h^{4/9}$. Combined with double-$λ$ halo mass function, the average BHMR ratio in all halos (~0.024 at z=0) can be analytically derived, along with its redshift evolution. The fraction of total baryons in all galaxies is ~7.6% at z=0 and increases with time $\propto t^{1/3}$. The SPARC (Spitzer Photometry \& Accurate Rotation Curves) data with 175 late-type galaxies were used for derivation and comparison.
