幽灵星系作为玻色-爱因斯坦暗物质的孤子
Ghostly Galaxies as Solitons of Bose-Einstein Dark Matter
摘要：
普通矮星系的巨大暗核无法用标准的重粒子解释暗物质。这一谜题因发现一个非常大但几乎不可见的、以暗物质为主的Antlia II星系而加剧，该星系是通过{ \t Gaia}卫星跟踪恒星运动而发现的。虽然Antlia II的质量很低，但它的可见半径是任何已知矮星系的两倍多，具有前所未有的低密度核心。我们发现Antlia II有利于暗物质作为一个玻色-爱因斯坦凝聚体，其中的基态是一个稳定的孤子的核心半径由德布罗意波长。星系质量越低，德布罗意波长越大，所以质量最小的星系应该有最宽的孤子核心和最低的密度。超轻玻色子为$m_ψ\sim 1.1 \times10^{-22}$ eV，很好地解释了Antlia II中大尺寸和缓慢移动的恒星，并与来自更大质量矮星系致密核心的玻色子质量估计一致。对于这个非常轻的玻色子，Antlia II接近于不确定原理所允许的星系形成的下限Jeans尺度，因此预计会有其他例子，但没有一个在尺寸上明显更大。对矮星系令人困惑的暗核心的这种简单解释意味着暗物质是一种超轻玻色子，就像弦论中的轴子一样。
英文摘要：
The large dark cores of common dwarf galaxies are unexplained by the standard heavy particle interpretation of dark matter. This puzzle is exacerbated by the discovery of a very large but barely visible, dark matter dominated galaxy Antlia II orbiting the Milky Way, uncovered by tracking star motions with the {\t Gaia} satellite. Although Antlia II has a low mass, its visible radius is more than double any known dwarf galaxy, with an unprecedentedly low density core. We show that Antlia II favors dark matter as a Bose-Einstein condensate, for which the ground state is a stable soliton with a core radius given by the de Broglie wavelength. The lower the galaxy mass, the larger the de Broglie wavelength, so the least massive galaxies should have the widest soliton cores of lowest density. An ultra-light boson of $m_ψ\sim 1.1 \times10^{-22}$ eV, accounts well for the large size and slowly moving stars within Antlia II, and agrees with boson mass estimates derived from the denser cores of more massive dwarf galaxies. For this very light boson, Antlia II is close to the lower limiting Jeans scale for galaxy formation permitted by the Uncertainty Principle, so other examples are expected but none significantly larger in size. This simple explanation for the puzzling dark cores of dwarf galaxies implies dark matter as an ultra-light boson, such as an axion generic in String Theory.
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