On the mass of ultra-light bosonic dark matter from galactic dynamics
On the mass of ultra-light bosonic dark matter from galactic dynamics
复制标题
从星系动力学论超轻玻色子暗物质的质量
DOI：
10.1088/1475-7516/2012/02/011
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
Icn Unam
中科院分区：
文献类型：
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作者：
V. Lora;J. Magaña;A. Bernal;F. J. Sánchez;E. K. G. U. Heidelberg;IA Unam;Icn Unam
我们考虑了银河系暗物质由超轻标量粒子组成的假设，并利用矮小球状星系的内部性质来确定这些玻色子粒子质量m的首选范围。我们重新研究了小熊座冷团的寿命问题，以及穹隆星团和矮椭圆星团球状星团的快速轨道衰变问题。将标量场晕看作一个刚性的背景引力势，利用N体模拟，研究了小熊座冷团的溶解时间标度与m的关系。结果表明，对于0.3×10~(-22)eV<；m<；1×10~(-22)eV范围内的标量场暗晕，没有自作用的标量场暗晕核将足够大，足以解释小熊座冷团的寿命和星座球状星团的广泛分布，但又足够小，使暗晕的质量与动力学极限相容。令人鼓舞的是，这个m的间隔与抑制银晕中子结构过剩所需的间隔一致，并与宇宙微波辐射的声学峰值相容。另一方面，对于耦合常数为L的自相互作用标量场，需要m^4/L<；=0.55×10~(-3)eV^4的值来解释这些矮小球状星系暗晕的性质。
We consider the hypothesis that galactic dark matter is composed of ultra-light scalar particles and use internal properties of dwarf spheroidal galaxies to establish a preferred range for the mass m of these bosonic particles. We re-investigate the problem of the longevity of the cold clump in Ursa Minor and the problem of the rapid orbital decay of the globular clusters in Fornax and dwarf ellipticals. Treating the scalar field halo as a rigid background gravitational potential and using N-body simulations, we have explored how the dissolution timescale of the cold clump in Ursa Minor depends on m. It is demonstrated that for masses in the range 0.3x10^-22 eV < m <1x10^-22 eV, scalar field dark halos without self-interaction would have cores large enough to explain the longevity of the cold clump in Ursa Minor and the wide distribution of globular clusters in Fornax, but small enough to make the mass of the dark halos compatible with dynamical limits. It is encouraging to see that this interval of m is consistent with that needed to suppress the overproduction of substructure in galactic halos and is compatible with the acoustic peaks of cosmic microwave radiation. On the other hand, for self-interacting scalar fields with coupling constant l, values of m^4/l <= 0.55x10^3 eV^4 are required to account for the properties of the dark halos of these dwarf spheroidal galaxies.